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Title: The Astronomy of Milton's 'Paradise Lost'

Author: Thomas Orchard

Release Date: March 29, 2009 [EBook #28434]

Language: English

Character set encoding: ISO-8859-1

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TRANSCRIBER'S NOTE


Greek letters used to identify stars (Bayer designation), are replaced
with the full name of the Greek letter, e.g. Alpha Centauri.

The single Greek word in the text is transliterated within braces, {komê}.

Minor punctuation and hyphenation inconsistencies have been corrected.

The spelling "Bernices" for "Berenices" has been retained throughout.

The following minor typographical errors have been corrected:
p75:  "establish" changed to "established"
p99:  "Firmanent" changed to "Firmament"
p111: "they thoughts" changed to "thy thoughts"
p120: "suen" changed to "seuen"
p134: "consequenc" changed to "consequence"
p146: "geographieal" changed to "geographical"
p167: "Lyrae" changed to "Lyræ" for consistency
p286: Removed redundant word "degrees" following the degree symbol




                THE ASTRONOMY
                     OF
           MILTON'S 'PARADISE LOST'




[Illustration: A TYPICAL SUN-SPOT]




                THE ASTRONOMY
                     OF
           MILTON'S 'PARADISE LOST'

                     BY

           THOMAS N. ORCHARD, M.D.

MEMBER OF THE BRITISH ASTRONOMICAL ASSOCIATION


_These are thy glorious works, Parent of good,
Almighty! thine this universal frame,
Thus wondrous fair: Thyself how wondrous then!
Unspeakable._


           LONGMANS, GREEN, AND CO.
         LONDON, NEW YORK, AND BOMBAY
                     1896

             All rights reserved




CONTENTS


CHAPTER                                                             PAGE
   I. A Short Historical Sketch of Astronomy                           1
  II. Astronomy in the Seventeenth Century                            45
 III. Milton's Astronomical Knowledge                                 81
  IV. Milton and Galileo                                             113
   V. The Seasons                                                    140
  VI. The Starry Heavens                                             152
 VII. The Starry Heavens                                             200
VIII. Description of Celestial Objects Mentioned in 'Paradise Lost'  244
  IX. Milton's Imaginative and Descriptive Astronomy                 306




ILLUSTRATIONS


_PLATES_

A Typical Sun-spot                                        _Frontispiece_
Venus on the Sun's Disc                               _To face page_  66
Cluster in Hercules                                          "       218
Great Nebula in Orion                                        "       230
A Portion of the Moon's Surface                              "       268


_IN TEXT_

FIG.                                                                PAGE
1.  The Ptolemaic System of the Universe                              86
2.  Milton's Division of Universal Space                              96
3.  A Binary Star System--70 Ophiuchi                                184
4.  The Orbits of the Components of Gamma Virginis                   189
5.  Apparent Orbit of the Companion of Sirius                        190
6.  A Sun-spot Magnified                                             247
7.  The Corona during the Eclipse of May 1883                        254
8.  A Portion of the Milky Way                                       289



PREFACE


Many able and cultured writers have delighted to expatiate on the
beauties of Milton's 'Paradise Lost,' and to linger with admiration over
the lofty utterances expressed in his poem. Though conscious of his
inability to do justice to the sublimest of poets and the noblest of
sciences, the author has ventured to contribute to Miltonic literature a
work which he hopes will prove to be of an interesting and instructive
character. Perhaps the choicest passages in the poem are associated with
astronomical allusion, and it is chiefly to the exposition and
illustration of these that this volume is devoted.

The writer is indebted to many authors for information and reference,
and especially to Miss Agnes M. Clerke, Professors Masson and Young, Mr.
James Nasmyth, Mr. G. F. Chambers, and Sir Robert Ball. Also to the
works of the late Mr. R. A. Proctor, Sirs W. and J. Herschel, Admiral
Smyth, Professor Grant, Mr. J. R. Hind, Sir David Brewster, Rev. A. B.
Whatton, and Prebendary Webb.

Most of the illustrations have been supplied by the Publishers: Messrs.
Macmillan and W. Hunt & Co. have kindly permitted the reproduction of
some of their drawings.

MANCHESTER, _March 1896_.




CHAPTER I

A SHORT HISTORICAL SKETCH OF ASTRONOMY


Astronomy is the oldest and most sublime of all the sciences. To a
contemplative observer of the heavens, the number and brilliancy of the
stars, the lustre of the planets, the silvery aspect of the Moon, with
her ever-changing phases, together with the order, the harmony, and
unison pervading them all, create in his mind thoughts of wonder and
admiration. Occupying the abyss of space indistinguishable from
infinity, the starry heavens in grandeur and magnificence surpass the
loftiest conceptions of the human mind; for, at a distance beyond the
range of ordinary vision, the telescope reveals clusters, systems,
galaxies, universes of stars--suns--the innumerable host of heaven, each
shining with a splendour comparable with that of our Sun, and, in all
likelihood, fulfilling in a similar manner the same beneficent purposes.

The time when man began to study the stars is lost in the antiquity of
prehistoric ages. The ancient inhabitants of the Earth regarded the
heavenly bodies with veneration and awe, erected temples in their
honour, and worshipped them as deities. Historical records of astronomy
carry us back several thousand years. During the greater part of this
time, and until a comparatively recent period, astronomy was associated
with astrology--a science which originated from a desire on the part of
mankind to penetrate the future, and which was based upon the supposed
influence of the heavenly bodies upon human and terrestrial affairs. It
was natural to imagine that the overruling power which governed and
directed the course of sublunary events resided in the heavens, and that
its decrees might be understood by watching the movements of the
heavenly bodies under its control. It was, therefore, believed that by
observing the configuration of the planets and the positions of the
constellations at the instant of the birth of an individual, his
horoscope, or destiny, could be foretold; and that by making
observations of a somewhat similar nature the occurrence of events of
public importance could be predicted. When, however, the laws which
govern the motions of the heavenly bodies became better known, and
especially after the discovery of the great law of gravitation,
astrology ceased to be a belief, though for long after it retained its
power over the imagination, and was often alluded to in the writings of
poets and other authors.

In the early dawn of astronomical science, the theories upheld with
regard to the structure of the heavens were of a simple and primitive
nature, and might even be described as grotesque. This need occasion no
surprise when we consider the difficulties with which ancient
astronomers had to contend in their endeavours to reduce to order and
harmony the complicated motions of the orbs which they beheld circling
around them.

The grouping of the stars into constellations having fanciful names,
derived from fable or ancient mythology, occurred at a very early
period, and though devoid of any methodical arrangement, is yet
sufficiently well-defined to serve the purposes of modern astronomers.
Several of the ancient nations of the earth, including the Chaldeans,
Egyptians, Hindus, and Chinese, claim to have been the earliest
astronomers. Chinese records of astronomy reveal an antiquity of near
3,000 years B.C., but they contain no evidence that their authors
possessed any scientific knowledge, and they merely record the
occurrence of solar eclipses and the appearances of comets.

It is not known when astronomy was first studied by the Egyptians; but
what astronomical information they have handed down is not of a very
intelligible kind, nor have they left behind any data that can be relied
upon. The Great Pyramid, judging from the exactness with which it faces
the cardinal points, must have been designed by persons who possessed a
good knowledge of astronomy, and it was probably made use of for
observational purposes.

It is now generally admitted that correct astronomical observations were
first made on the plains of Chaldea, records of eclipses having been
discovered in Chaldean cities which date back 2,234 years B.C. The
Chaldeans were true astronomers: they made correct observations of the
risings and settings of the heavenly bodies; and the exact orientation
of their temples and public buildings indicates the precision with which
they observed the positions of celestial objects. They invented the
zodiac and gnomon, made use of several kinds of dials, notified
eclipses, and divided the day into twenty-four hours.

To the Greeks belongs the credit of having first studied astronomy in a
regular and systematic manner. THALES (640 B.C.) was one of the earliest
of Greek astronomers, and may be regarded as the founder of the science
among that people. He was born at Miletus, and afterwards repaired to
Egypt for the purpose of study. On his return to Greece he founded the
Ionian school, and taught the sphericity of the Earth, the obliquity of
the ecliptic, and the true causes of eclipses of the Sun and Moon. He
also directed the attention of mariners to the superiority of the Lesser
Bear, as a guide for the navigation of vessels, as compared with the
Great Bear, by which constellation they usually steered. Thales believed
the Earth to be the centre of the universe, and that the stars were
composed of fire; he also predicted the occurrence of a great solar
eclipse.

Thales had for his successors Anaximander, Anaximenes, and Anaxagoras,
who taught the doctrines of the Ionian school.

The next great astronomer that we read of is PYTHAGORAS, who was born at
Samos 590 B.C. He studied under Thales, and afterwards visited Egypt and
India, in order that he might make himself familiar with the scientific
theories adopted by those nations. On his return to Europe he founded
his school in Italy, and taught in a more extended form the doctrines of
the Ionian school. In his speculations with regard to the structure of
the universe he propounded the theory (though the reasons by which he
sustained it were fanciful) that the Sun is the centre of the planetary
system, and that the Earth revolves round him. This theory--the accuracy
of which has since been confirmed--received but little attention from
his successors, and it sank into oblivion until the time of Copernicus,
by whom it was revived. Pythagoras discovered that the Morning and
Evening Stars are one and the same planet.

Among the famous astronomers who lived about this period we find
recorded the names of Meton, who introduced the Metonic cycle into
Greece and erected the first sundial at Athens; Eudoxus, who persuaded
the Greeks to adopt the year of 365-1/4 days; and Nicetas, who taught
that the Earth completed a daily revolution on her axis.

The Alexandrian school, which flourished for three centuries prior to
the Christian era, produced men of eminence whose discoveries and
investigations, when arranged and classified, enabled astronomy to be
regarded as a true theoretical science. The positions of the fixed stars
and the paths of the planets were determined with greater accuracy, and
irregularities of the motions of the Sun and Moon were investigated with
greater precision. Attempts were made to ascertain the distance of the
Sun from the Earth, and also the dimensions of the terrestrial sphere.
The obliquity of the ecliptic was accurately determined, and an arc of
the meridian was measured between Syene and Alexandria. The names of
Aristarchus, Eratosthenes, Aristyllus, Timocharis, and Autolycus, are
familiarly known in association with the advancement of the astronomy of
this period.

We now reach the name of HIPPARCHUS of Bithynia (140 B.C.), the most
illustrious astronomer of antiquity, who did much to raise astronomy to
the position of a true science, and who has also left behind him ample
evidence of his genius 'as a mathematician, an observer, and a
theorist.' We are indebted to him for the earliest star catalogue, in
which he included 1,081 stars. He discovered the Precession of the
Equinoxes, and determined the motions of the Sun and Moon, and also the
length of the year, with greater precision than any of his predecessors.
He invented the sciences of plane and spherical trigonometry, and was
the first to use right ascensions and declinations.

The next astronomer of eminence after Hipparchus was PTOLEMY (130 A.D.),
who resided at Alexandria. He was skilled as a mathematician and
geographer, and also excelled as a musician. His chief discovery was an
irregularity of the lunar motion, called the '_evection_.' He was also
the first to observe the effect of the refraction of light in causing
the apparent displacement of a heavenly body from its true position.
Ptolemy devoted much of his time to extending and improving the theories
of Hipparchus, and compiled a great treatise, called the 'Almagest,'
which contains nearly all the knowledge we possess of ancient astronomy.
Ptolemy's name is, however, most widely known in association with what
is called the Ptolemaic theory. This system, which originated long
before his time, but of which he was one of the ablest expounders, was
an attempt to establish on a scientific basis the conclusions and
results arrived at by early astronomers who studied and observed the
motions of the heavenly bodies. Ptolemy regarded the Earth as the
immovable centre of the universe, round which the Sun, Moon, planets,
and the entire heavens completed a daily revolution in twenty-four
hours. After the death of Ptolemy no worthy successor was found to
occupy his place, the study of astronomy began to decline among the
Greeks, and after a time it ceased to be cultivated by that people.

The Arabs next took up the study of astronomy, which they prosecuted
most assiduously for a period of four centuries. Their labours were,
however, confined chiefly to observational work, in which they
excelled; unlike their predecessors, they paid but little attention to
speculative theories--indeed, they regarded with such veneration the
opinions held by the Greeks, that they did not feel disposed to question
the accuracy of their doctrines. The most eminent astronomer among the
Arabs was ALBATEGNIUS (680 A.D.). He corrected the Greek observations,
and made several discoveries which testified to his abilities as an
observer. IBN YUNIS and ABUL WEFU were Arab astronomers who earned a
high reputation on account of the number and accuracy of their
observations. In Persia, a descendant of the famous Genghis Khan erected
an observatory, where astronomical observations were systematically
made. Omar, a Persian astronomer, suggested a reformation of the
calendar which, if it had been adopted, would have insured greater
accuracy than can be attained by the Gregorian style now in use. In
1433, Ulugh Beg, who resided at Samarcand, made many observations, and
constructed a star catalogue of greater exactness than was known to
exist prior to his time. The Arabs may be regarded as having been the
custodians of astronomy until the time of its revival in another quarter
of the Globe.

After the lapse of many centuries, astronomy was introduced into Western
Europe in 1220, and from that date to the present time its career has
been one of triumphant progress. In 1230, a translation of Ptolemy's
'Almagest' from Arabic into Latin was accomplished by order of the
German Emperor, Frederick II.; and in 1252 Alphonso X., King of Castile,
himself a zealous patron of astronomy, caused a new set of astronomical
tables to be constructed at his own expense, which, in honour of his
Majesty, were called the 'Alphonsine Tables.' Purbach and Regiomontanus,
two German astronomers of distinguished reputation, and Waltherus, a man
of considerable renown, made many important observations in the
fifteenth century.

The most eminent astronomer who lived during the latter part of this
century was Copernicus. NICOLAS COPERNICUS was born February 19, 1473,
at Thorn, a small town situated on the Vistula, which formed the
boundary between the kingdoms of Prussia and Poland. His father was a
Polish subject, and his mother of German extraction. Having lost his
parents early in life, he was educated under the supervision of his
uncle Lucas, Bishop of Ermland. Copernicus attended a school at Thorn,
and afterwards entered the University of Cracow, in 1491, where he
devoted four years to the study of mathematics and science. On leaving
Cracow he attached himself to the University of Bologna as a student of
canon law, and attended a course of lectures on astronomy given by
Novarra. In the ensuing year he was appointed canon of Frauenburg, the
cathedral city of the Diocese of Ermland, situated on the shores of the
Frisches Haff. In the year 1500 he was at Rome, where he lectured on
mathematics and astronomy. He next spent a few years at the University
of Padua, where, besides applying himself to mathematics and astronomy,
he studied medicine and obtained a degree. In 1505 Copernicus returned
to his native country, and was appointed medical attendant to his uncle,
the Bishop of Ermland, with whom he resided in the stately castle of
Heilsberg, situated at a distance of forty-six miles from Frauenburg.
Copernicus lived with his uncle from 1507 till 1512, and during that
time prosecuted his astronomical studies, and undertook, besides, many
arduous duties associated with the administration of the diocese; these
he faithfully discharged until the death of the Bishop, which occurred
in 1512. After the death of his uncle he took up his residence at
Frauenburg, where he occupied his time in meditating on his new
astronomy and undertaking various duties of a public character, which he
fulfilled with credit and distinction. In 1523 he was appointed
Administrator-General of the diocese. Though a canon of Frauenburg,
Copernicus never became a priest.

After many years of profound meditation and thought, Copernicus, in a
treatise entitled 'De Revolutionibus Orbium Celestium,' propounded a new
theory, or, more correctly speaking, revived the ancient Pythagorean
system of the universe. This great work, which he dedicated to Pope Paul
III., was completed in 1530; but he could not be prevailed upon to have
it published until 1543, the year in which he died. In 1542 Copernicus
had an apoplectic seizure, followed by paralysis and a gradual decay of
his mental and vital powers. His book was printed at Nuremberg, and the
first copy arrived at Frauenburg on May 24, 1543, in time to be touched
by the hands of the dying man, who in a few hours after expired. The
house in which Copernicus lived at Allenstein is still in existence, and
in the walls of his chamber are visible the perforations which he made
for the purpose of observing the stars cross the meridian.

Copernicus was the means of creating an entire revolution in the science
of astronomy, by transferring the centre of our system from the Earth to
the Sun. He accounted for the alternation of day and night by the
rotation of the Earth on her axis, and for the vicissitudes of the
seasons by her revolution round the Sun. He devoted the greater part of
his life to meditating on this theory, and adduced several weighty
reasons in its support. Copernicus could not help perceiving the
complications and entanglements by which the Ptolemaic system of the
universe was surrounded, and which compared unfavourably with the simple
and orderly manner in which other natural phenomena presented themselves
to his observation. By perceiving that Mars when in opposition was not
much inferior in lustre to Jupiter, and when in conjunction resembled a
star of the second magnitude, he arrived at the conclusion that the
Earth could not be the centre of the planet's motion. Having discovered
in some ancient manuscripts a theory, ascribed to the Egyptians, that
Mercury and Venus revolved round the Sun, whilst they accompanied the
orb in his revolution round the Earth, Copernicus was able to perceive
that this afforded him a means of explaining the alternate appearance of
those planets on each side of the Sun. The varied aspects of the
superior planets, when observed in different parts of their orbits, also
led him to conclude that the Earth was not the central body round which
they accomplished their revolutions. As a combined result of his
observation and reasoning Copernicus propounded the theory that the Sun
is the centre of our system, and that all the planets, including the
Earth, revolve in orbits around him. This, which is called the
Copernican system, is now regarded as, and has been proved to be, the
true theory of the solar system.

TYCHO BRAHÉ was a celebrated Danish astronomer, who earned a deservedly
high reputation on account of the number and accuracy of his
astronomical observations and calculations. The various astronomical
tables that were in use in his time contained many inaccuracies, and it
became necessary that they should be reconstructed upon a more correct
basis. Tycho possessed the practical skill required for this kind of
work.

He was born December 14, 1546, at Knudstorp, near Helsingborg. His
father, Otto Brahé, traced his descent from a Swedish family of noble
birth. At the age of thirteen Tycho was sent to the University of
Copenhagen, where it was intended he should prepare himself for the
study of the law.

The prediction of a great solar eclipse, which was to happen on August
21, 1560, caused much public excitement in Denmark, for in those days
such phenomena were regarded as portending the occurrence of events of
national importance. Tycho looked forward with great eagerness to the
time of the eclipse. He watched its progress with intense interest, and
when he perceived all the details of the phenomenon occur exactly as
they were predicted, he resolved to pursue the study of a science by
which, as was then believed, the occurrence of future events could be
foretold. From Copenhagen Tycho Brahé was sent to Leipsic to study
jurisprudence, but astronomy absorbed all his thoughts. He spent his
pocket-money in purchasing astronomical books, and, when his tutor had
retired to sleep, he occupied his time night after night in watching the
stars and making himself familiar with their courses. He followed the
planets in their direct and retrograde movements, and with the aid of a
small globe and pair of compasses was able by means of his own
calculations to detect serious discrepancies in the Alphonsine and
Prutenic tables. In order to make himself more proficient in calculating
astronomical tables he studied arithmetic and geometry, and learned
mathematics without the aid of a master. Having remained at Leipsic for
three years, during which time he paid far more attention to the study
of astronomy than to that of law, he returned to his native country in
consequence of the death of an uncle, who bequeathed him a considerable
estate. In Denmark he continued to prosecute his astronomical studies,
and incurred the displeasure of his friends, who blamed him for
neglecting his intended profession and wasting his time on astronomy,
which they regarded as useless and unprofitable.

Not caring to remain among his relatives, Tycho Brahé returned to
Germany, and arrived at Wittenberg in 1566. Whilst residing here he had
an altercation with a Danish gentleman over some question in
mathematics. The quarrel led to a duel with swords, which terminated
rather unfortunately for Tycho, who had a portion of his nose cut off.
This loss he repaired by ingeniously contriving one of gold, silver, and
wax, which was said to bear a good resemblance to the original. From
Wittenberg Tycho proceeded to Augsburg, where he resided for two years.
Here he made the acquaintance of several men distinguished for their
learning and their love of astronomy. During his stay at Augsburg he
constructed a quadrant of fourteen cubits radius, on which were
indicated the single minutes of a degree; he made many valuable
observations with this instrument, which he used in combination with a
large sextant.

In 1571 Tycho returned to Denmark, where his fame as an astronomer had
preceded him, and was the means of procuring for him a hearty welcome
from his relatives and friends. In 1572, when returning one night from
his laboratory--for Tycho studied alchemy as well as astronomy--he
beheld what appeared to be a new and brilliant star in the
constellation Cassiopeia, which was situated overhead. He directed the
attention of his companions to this wonderful object, and all declared
that they had never observed such a star before. On the following night
he measured its distance from the nearest stars in the constellation,
and arrived at the conclusion that it was a fixed star, and beyond our
system.

This remarkable object remained visible for sixteen months, and when at
its brightest rivalled Sirius. At first it was of a brilliant white
colour, but as it diminished in size it became yellow; it next changed
to a red colour, resembling Aldebaran; afterwards it appeared like
Saturn, and as it grew smaller it decreased in brightness, until it
finally became invisible. In 1573 Tycho Brahé married a peasant-girl
from the village of Knudstorp. This imprudent act roused the resentment
of his relatives, who, being of noble birth, were indignant that he
should have contracted such an alliance. The bitterness and mutual
ill-feeling created by this affair became so intense that the King of
Denmark deemed it advisable to endeavour to bring about a
reconciliation.

After this Tycho returned to Germany, and visited several cities before
deciding where he should take up his permanent residence.

His fame as an astronomer was now so great that he was received with
distinction wherever he went, and on the occasion of a visit to
Hesse-Cassel he spent a few pleasant days with William, Landgrave of
Hesse, who was himself skilled in astronomy.

Frederick II., King of Denmark, having recognised Tycho Brahé's great
merits as an astronomer, and not wishing that his fame should add lustre
to a foreign Court, expressed a desire that he should return to his
native country, and as an inducement offered him a life interest in the
island of Huen, in the Sound, where he undertook to erect and equip an
observatory at his own expense; the King also promised to bestow upon
him a pension, and grant him other emoluments besides.

Tycho gladly accepted this generous offer, and during the construction
of the observatory occupied his time in making a magnificent collection
of instruments and appliances adapted for observational purposes. This
handsome edifice, upon which the King of Denmark expended a sum of
20,000_l._, was called 'Uranienburg' ('The Citadel of the Heavens').
Here Tycho resided for a period of twenty years, during which time he
pursued his astronomical labours with untiring energy and zeal, and made
a large number of observations and calculations of much superior
accuracy to any that existed previously, which were afterwards of great
service to his successors. During his long residence at Huen, Tycho was
visited by many distinguished persons, who were attracted to his island
home by his fame and the magnificence of his observatory. Among them was
James VI. of Scotland, who, whilst journeying to the Court of Denmark
on the occasion of his marriage to a Danish princess, paid Tycho a
visit, and enjoyed his hospitality for a week. The King was delighted
with all that he saw, and on his departure presented Tycho with a
handsome donation, and at his request composed some Latin verses, in
which he eulogised his host and praised his observatory.

The island of Huen is situated about six miles from the coast of
Zealand, and fourteen from Copenhagen. It has a circumference of six
miles, and consists chiefly of an elevated plateau, in the centre of
which Tycho erected his observatory, the site of which is now marked by
two pits and a few mounds of earth--all that remains of Uranienburg. All
went well with Tycho Brahé during the lifetime of his noble patron; but
in 1588 Frederick II. died, and was succeeded by his son, a youth eleven
years of age.

The Danish nobles had long been jealous of Tycho's fame and reputation,
and on the death of the King an opportunity was afforded them of
intriguing with the object of accomplishing his downfall. Several false
accusations were brought against him, and the Court party made the
impoverished state of the Treasury an excuse for depriving him of his
pension and emoluments granted by the late King.

Tycho was no longer able to bear the expense of maintaining his
establishment at Huen, and fearing that he might be deprived of the
island itself, he took a house in Copenhagen, to which he removed all
his smaller instruments.

During his residence in the capital he was subjected to annoyance and
persecution. An order was issued in the King's name preventing him from
carrying on his chemical experiments, and he besides suffered the
indignity of a personal assault. Tycho Brahé resolved to quit his
ungrateful country and seek a home in some foreign land, where he should
be permitted to pursue his studies unmolested and live in quietness and
peace. He accordingly removed from the island of Huen all his
instruments and appliances that were of a portable nature, and packed
them on board a vessel which he hired for the purpose of transport, and,
having embarked with his family, his servants, and some of his pupils
and assistants, 'this interesting barque, freighted with the glory of
Denmark,' set sail from Copenhagen about the end of 1597, and having
crossed the Baltic in safety, arrived at Rostock, where Tycho found some
old friends waiting to receive him. He was now in doubt as to where he
should find a home, when the Austrian Emperor Rudolph, himself a liberal
patron of science and the fine arts, having heard of Tycho Brahé's
misfortunes, sent him an invitation to take up his abode in his
dominions, and promised that he should be treated in a manner worthy of
his reputation and fame.

Tycho resolved to accept the Emperor's kind invitation, and in the
spring of 1599 arrived at Prague, where he found a handsome residence
prepared for his reception.

He was received by the Emperor in a most cordial manner and treated with
the greatest kindness. An annual pension of three thousand crowns was
settled upon him for life, and he was to have his choice of several
residences belonging to his Majesty, where he might reside and erect a
new observatory. From among these he selected the Castle of Benach, in
Bohemia, which was situated on an elevated plateau and commanded a wide
view of the horizon.

During his residence at Benach Tycho received a visit from Kepler, who
stayed with him for several months in order that he might carry out some
astronomical observations. In the following year Kepler returned, and
took up his permanent residence with Tycho, having been appointed
assistant in his observatory, a post which, at Tycho's request, was
conferred upon him by the Emperor.

Tycho Brahé soon discovered that his ignorance of the language and
unfamiliarity with the customs of the people caused him much
inconvenience. He therefore asked permission from the Emperor to be
allowed to remove to Prague. This request was readily granted, and a
suitable residence was provided for him in the city.

In the meantime his family, his large instruments, and other property,
having arrived at Prague, Tycho was soon comfortably settled in his new
home.

Though Tycho Brahé continued his astronomical observations, yet he could
not help feeling that he lived among a strange people; nor did the
remembrance of his sufferings and the cruel treatment he received at the
hands of his fellow-countrymen subdue the affection which he cherished
towards his native land. Pondering over the past, he became despondent
and low-spirited; a morbid imagination caused him to brood over small
troubles, and gloomy, melancholy thoughts possessed his mind--symptoms
which seemed to presage the approach of some serious malady. One
evening, when visiting at the house of a friend, he was seized with a
painful illness, to which he succumbed in less than a fortnight. He died
at Prague on October 24, 1601, when in his fifty-fifth year.

The Emperor Rudolph, when informed of Tycho Brahé's death, expressed his
deep regret, and commanded that he should be interred in the principal
church in the city, and that his obsequies should be celebrated with
every mark of honour and respect.

Tycho Brahé stands out as the most romantic and prominent figure in the
history of astronomy. His independence of character, his ardent
attachments, his strong hatreds, and his love of splendour, are
characteristics which distinguish him from all other men of his age.
This remarkable man was an astronomer, astrologer, and alchemist; but in
his latter years he renounced astrology, and believed that the stars
exercised no influence over the destinies of mankind.

As a practical astronomer, Tycho Brahé has not been excelled by any
other observer of the heavens. The magnificence of his observatory at
Huen, upon the equipment and embellishment of which it is stated he
expended a ton of gold; the splendour and variety of his instruments,
and his ingenuity in inventing new ones, would alone have made him
famous. But it was by the skill and assiduity with which he carried out
his numerous and important observations that he has earned for himself a
position of the most honourable distinction among astronomers. In his
investigation of the Lunar theory Tycho Brahé discovered the Moon's
_annual equation_, a yearly effect produced by the Sun's disturbing
force as the Earth approaches or recedes from him in her orbit. He also
discovered another inequality in the Moon's motion, called the
_variation_. He determined with greater exactness astronomical
refractions from an altitude of 45° downwards to the horizon, and
constructed a catalogue of 777 stars. He also made a vast number of
observations on planets, which formed the basis of the 'Rudolphine
Tables,' and were of invaluable assistance to Kepler in his
investigation of the laws relating to planetary motion.

Tycho Brahé declined to accept the Copernican theory, and devised a
system of his own, which he called the 'Tychonic.' By this arrangement
the Earth remained stationary, whilst all the planets revolved round
the Sun, who in his turn completed a daily revolution round the Earth.
All the phenomena associated with the motions of those bodies could be
explained by means of this system; but it did not receive much support,
and after the Copernican theory became better understood it was given
up, and heard of no more.

We now arrive at the name of KEPLER, one of the very greatest of
astronomers, and a man of remarkable genius, who was the first to
discover the real nature of the paths pursued by the Earth and planets
in their revolution round the Sun. After seventeen years of close
observation, he announced that those bodies travelled round the Sun in
elliptical or oval orbits, and not in circular paths, as was believed by
Copernicus. In his investigation of the laws which govern the motions of
the planets he formulated those famous theorems known as 'Kepler's
Laws,' which will endure for all time as a proof of his sagacity and
surpassing genius. Prior to the discovery of those laws the Sun, though
acknowledged to be the centre of the system, did not appear to occupy a
central position as regards the motions of the planets; but Kepler, by
demonstrating that the planes of the orbits of all the planets, and the
lines connecting their apsides, passed through the Sun, was enabled to
assign the orb his true position with regard to those bodies.

JOHN KEPLER was born at Weil, in the Duchy of Wurtemberg, December 21,
1571. His parents, though of noble family, lived in reduced
circumstances, owing to causes for which they were themselves chiefly
responsible. In his youth Kepler suffered so much from ill-health that
his education had to be neglected. In 1586 he was sent to a monastic
school at Maulbronn, which had been established at the Reformation, and
was under the patronage of the Duke of Wurtemberg. Afterwards he studied
at the University of Tubingen, where he distinguished himself and took a
degree. Kepler devoted his attention chiefly to science and mathematics,
but paid no particular attention to the study of astronomy. Maestlin,
the professor of mathematics, whose lectures he attended, upheld the
Copernican theory, and Kepler, who adopted the views of his teacher,
wrote an essay in favour of the diurnal rotation of the Earth, in which
he supported the more recent astronomical doctrines. In 1594, a vacancy
having occurred in the professorship of astronomy at Gratz consequent
upon the death of George Stadt, Kepler was appointed his successor. He
did not seek this office, as he felt no particular desire to take up the
study of astronomy, but was recommended by his tutors as a man well
fitted for the post. He was thus in a manner compelled to devote his
time and talents to the science of astronomy. Kepler directed his
attention to three subjects--viz. 'the number, the size, and the motion
of the orbits of the planets.' He endeavoured to ascertain if any
regular proportion existed between the sizes of the planetary orbits, or
in the difference of their sizes, but in this he was unsuccessful. He
then thought that, by imagining the existence of a planet between Mars
and Jupiter, and another between Venus and Mercury, he might be able to
attain his object; but he found that this assumption afforded him no
assistance. Kepler then imagined that as there were five regular
geometrical solids, and five planets, the distances of the latter were
regulated by the size of the solids described round one another. The
discovery afterwards of two additional planets testified to the
absurdity of this speculation. A description of these extraordinary
researches was published, in 1596, in a work entitled 'Prodromus of
Cosmographical Dissertations; containing the cosmographical mystery
respecting the admirable proportion of the celestial orbits, and the
genuine and real causes of the number, magnitude, and periods of the
planets, demonstrated by the five regular geometrical solids.' This
volume, notwithstanding the fanciful speculations which it contained,
was received with much favour by astronomers, and both Tycho Brahé and
Galileo encouraged Kepler to continue his researches. Galileo admired
his ingenuity, and Tycho advised him 'to lay a solid foundation for his
views by actual observation, and then, by ascending from these, to
strive to reach the causes of things.' Kepler spent many years in these
fruitless endeavours before he made those grand discoveries in search of
which he laboured so long.

The religious dissensions which at this time agitated Germany were
accompanied in many places by much tumult and excitement. At Gratz the
Catholics threatened to expel the Protestants from the city. Kepler, who
was of the Reformed faith, having recognised the danger with which he
was threatened, retired to Hungary with his wife, whom he had recently
married, and remained there for near twelve months, during which time he
occupied himself with writing several short treatises on subjects
connected with astronomy. In 1599 he returned to Gratz and resumed his
professorship.

In the year 1600 Kepler set out to pay Tycho Brahé a visit at Prague, in
order that he might be able to avail himself of information contained in
observations made by Tycho with regard to the eccentricities of the
orbits of the planets. He was received by Tycho with much cordiality,
and stayed with him for four months at his residence at Benach, Tycho in
the meantime having promised that he would use his influence with the
Emperor Rudolph to have him appointed as assistant in his observatory.
On the termination of his visit Kepler returned to Gratz, and as there
was a renewal of the religious trouble in the city, he resigned his
professorship, from which he only derived a small income, and, relying
on Tycho's promise, he again journeyed to Prague, and arrived there in
1601. Kepler was presented to the Emperor by Tycho, and the post of
Imperial Mathematician was conferred upon him, with a salary of 100
florins a year, upon condition that he should assist Tycho in his
observatory. This appointment was of much value to Kepler, because it
afforded him an opportunity of obtaining access to the numerous
astronomical observations made by Tycho, which were of great assistance
to him in the investigation of the subject which he had chosen--viz. the
laws which govern the motions of the planets, and the form and size of
the planetary orbits.

As an acknowledgment of the Emperor's great kindness, the two
astronomers resolved to compute a new set of astronomical tables, and in
honour of his Majesty they were to be called the 'Rudolphine Tables.'
This project pleased the Emperor, who promised to defray the expense of
their publication. Logomontanus, Tycho's chief assistant, had entrusted
to him that portion of the work relating to observations on the stars,
and Kepler had charge of the part which embraced the calculations
belonging to the planets and their orbits. This important work had
scarcely been begun when the departure of Logomontanus, who obtained an
appointment in Denmark, and the death of Tycho Brahé in October 1601,
necessitated its suspension for a time. Kepler was appointed Chief
Mathematician to the Emperor in succession to Tycho--a position of
honour and distinction, and to which was attached a handsome salary,
that was paid out of the Imperial treasury. But owing to the continuance
of expensive wars, which entailed a severe drain upon the resources of
the country, the public funds became very low, and Kepler's salary was
always in arrear. This condition of things involved him in serious
pecuniary difficulties, and the responsibility of having to maintain an
increasing family added to his anxieties. It was with the greatest
difficulty that he succeeded in obtaining payment of even a portion of
his salary, and he was reduced to such straits as to be under the
necessity of casting nativities in order to obtain money to meet his
most pressing requirements.

In 1609 Kepler published his great work, entitled 'The New Astronomy;
or, Commentaries on the Motions of Mars.' It was by his observation of
Mars, which has an orbit of greater eccentricity than that of any of the
other planets, with the exception of Mercury, that he was enabled, after
years of patient study, to announce in this volume the discovery of two
of the three famous theorems known as Kepler's Laws. The first is, that
all the planets move round the Sun in elliptic orbits, and that the orb
occupies one of the foci. The second is, that the radius-vector, or
imaginary line joining the centre of the planet and the centre of the
Sun, describes equal areas in equal times. The third law, which relates
to the connection between the periodic times and the distances of the
planets, was not discovered until ten years later, when Kepler, in 1619,
issued another work, called the 'Harmonies of the World,' dedicated to
James I. of England, in which was contained this remarkable law. These
laws have elevated astronomy to the position of a true physical science,
and also formed the starting-point of Newton's investigations which led
to the discovery of the law of gravitation. Kepler's delight on the
discovery of his third law was unbounded. He writes: 'Nothing holds me.
I will indulge in my sacred fury. I will triumph over mankind by the
honest confession that I have stolen the golden vases of the Egyptians
to build up a tabernacle for my God far away from the confines of Egypt.
If you forgive me, I rejoice; if you are angry, I can bear it. The die
is cast; the book is written, to be read either now or by posterity I
care not which. It may well wait a century for a reader, as God has
waited six thousand years for an observer.'

When Kepler presented his celebrated book to the Emperor, he remarked
that it was his intention to make a similar attack upon the other
planets, and promised that he would be successful if his Majesty would
undertake to find the means necessary for carrying on operations. But
the Emperor had more formidable enemies to contend with nearer home than
Jupiter and Saturn, and no funds were forthcoming to assist Kepler in
his undertaking.

The chair of mathematics in the University of Linz having become vacant,
Kepler offered himself as a candidate for the appointment, which he was
anxious to obtain; but the Emperor Rudolph was averse to his leaving
Prague, and encouraged him to hope that the arrears of his salary would
be paid. But past experience led Kepler to have no very sanguine
expectations on this point; nor was it until after the death of Rudolph,
in 1612, that he was relieved from his pecuniary embarrassments.

On the accession of Rudolph's brother, Matthias, to the Austrian throne,
Kepler was reappointed Imperial Mathematician; he was also permitted to
hold the professorship at Linz, to which he had been elected. Kepler was
not loth to remove from Prague, where he had spent eleven years harassed
by poverty and other domestic afflictions. Having settled with his
family at Linz, Kepler issued another work, in 1618, entitled 'Epitome
of the Copernican Astronomy,' in which he gave a general account of his
astronomical observations and discoveries, and a summary of his opinions
with regard to the theories which in those days were the subject of
controversial discussion. Almost immediately after its publication it
was included by the Congregation of the Index, at Rome, in the list of
prohibited books. This occasioned Kepler considerable alarm, as he
imagined it might interfere with the sale of his works, or give rise to
difficulties in the issue of others. He, however, was assured by his
friend Remus that the action of the Papal authorities need cause him no
anxiety.

The Emperor Matthias died in 1619, and was succeeded by Ferdinand III.,
who not only retained Kepler in his office, but gave orders that all the
arrears of his salary should be paid, including those which accumulated
during the reign of Rudolph; he also expressed a desire that the
'Rudolphine Tables' should be published without delay and at his cost.
But other obstacles intervened, for at this time Germany was involved in
a civil and religious war, which interfered with all peaceful
vocations. Kepler's library at Linz was sealed up by order of the
Jesuits, and the city was for a time besieged by troops. This state of
public affairs necessitated a considerable delay in the publication of
the 'Tables.'

The 'Rudolphine Tables' were published at Ulm in 1627. They were
commenced by Tycho Brahé, and completed by Kepler, who made his
calculations from Tycho's observations, and based them upon his own
great discovery of the ellipticity of the orbits of the planets. They
are divided into four parts. The first and third parts contain
logarithmic and other tables for the purpose of facilitating
astronomical calculations; in the second are tables of the Sun, Moon,
and planets; and in the fourth are indicated the positions of one
thousand stars as determined by Tycho. Kepler made a special journey to
Prague in order to present the 'Tables' to the Emperor, and afterwards
the Grand Duke of Tuscany sent him a gold chain as an acknowledgment of
his appreciation of the completion of this great work.

Albert Wallenstein, Duke of Friedland, an accomplished scholar and a man
fond of scientific pursuits, made Kepler a most liberal offer if he
would take up his residence in his dominions. After duly considering
this proposal, Kepler decided to accept the Duke's offer, provided it
received the sanction of the Emperor. This was readily given, and
Kepler, in 1629, removed with his family from Linz to Sagan, in Silesia.
The Duke of Friedland treated him with great kindness and liberality,
and through his influence he was appointed to a professorship in the
University of Rostock. Though Kepler was permitted to retain the pension
bestowed upon him by the late Emperor Rudolph, he was unable after his
removal to Silesia to obtain payment of it, and there was a large
accumulation of arrears. In a final endeavour to recover the amount
owing to him he travelled to Ratisbon, and appealed to the Imperial
Assembly, but without success. The fatigue which Kepler endured on his
journey, combined with vexation and disappointment, brought on a fever,
which terminated fatally. He died on November 15, 1630, when in the
sixtieth year of his age, and was interred in St. Peter's churchyard,
Ratisbon.

Kepler was a man of indomitable energy and perseverance, and spared
neither time nor trouble in the accomplishment of any object which he
took in hand. In thinking over the form of the orbits of the planets, he
writes: 'I brooded with the whole energy of my mind on this
subject--asking why they are not other than they are--the number, the
size, and the motions of the orbits.' But many fanciful ideas passed
through Kepler's imaginative brain before he hit upon the true form of
the planetary orbits. In his 'Mysterium Cosmographicum' he asserts that
the five kinds of regular polyhedral solids, when described round one
another, regulated the distances of the planets and size of the
planetary orbits. In support of this theory he writes as follows: 'The
orbit of the Earth is the measure of the rest. About it circumscribe a
dodecahedron. The sphere including this will be that of Mars. About
Mars' orbit describe a tetrahedron; the sphere containing this will be
Jupiter's orbit. Round Jupiter's describe a cube; the sphere including
this will be Saturn's. Within the Earth's orbit inscribe an icosahedron;
the sphere inscribed in it will be Venus's orbit. In Venus inscribe an
octahedron; the sphere inscribed in it will be Mercury's.'

The above quotation is an instance of Kepler's wild and imaginative
genius, which ultimately led him to make those sublime discoveries
associated with planetary motion which are known as 'Kepler's Laws.'

He describes himself as 'troublesome and choleric in politics and
domestic matters;' but in his relations with scientific men he was
affable and pleasant. He showed no jealousy of a rival, and was always
ready to recognise merit in others; nor did he hesitate to acknowledge
any error of his own when more recent discoveries proved that he was
wrong.

Some of his works contain passages, written in a jocular strain,
indicative of a bright and cheerful temperament. The following
characteristic paragraph refers to the opinions of the Epicureans with
regard to the appearance of a new star, which they ascribed to a
fortuitous concourse of atoms: 'When I was a youth, with plenty of idle
time on my hands, I was much taken with the vanity, of which some grown
men are not ashamed, of making anagrams by transposing the letters of my
name written in Latin so as to make another sentence. Out of Ioannes
Keplerus came _Serpens in akuleo_ (a serpent in his sting); but not
being satisfied with the meaning of these words, and being unable to
make another, I trusted the thing to chance, and, taking out of a pack
of playing-cards as many as there were letters in the name, I wrote one
upon each, and then began to shuffle them, and at each shuffle to read
them in the order they came, to see if any meaning came of it. Now, may
all the Epicurean gods and goddesses confound this same chance, which,
although I have spent a good deal of time over it, never showed me
anything like sense, even from a distance. So I gave up my cards to the
Epicurean eternity, to be carried away into infinity; and it is said
they are still flying about there, in the utmost confusion, among the
atoms, and have never yet come to any meaning. I will tell those
disputants, my opponents, not my own opinion, but my wife's. Yesterday,
when weary with writing, and my mind quite dusty with considering these
atoms, I was called to supper, and a salad I had asked for was set
before me. "It seems, then," said I aloud, "that if pewter dishes,
leaves of lettuce, grains of salt, drops of water, vinegar and oil, and
slices of egg, had been flying about in the air from all eternity, it
might at last happen by chance that there would come a salad." "Yes,"
says my wife, "but not so nice and well dressed as this of mine is."'

Notwithstanding the frequent interruptions which, owing to various
reasons, retarded his labours, Kepler was able to bring to a successful
completion the numerous and important works upon which he was engaged
during his lifetime, the voluminous nature of which may be imagined when
it is stated that he published thirty-three separate works, besides
leaving behind twenty-two volumes of manuscript.

During his researches on the motions of Mars, Kepler discovered that the
planet sometimes travelled at an accelerated rate of speed, and at
another time its pace was diminished. At one time he observed it to be
in advance of the place where he calculated it should be found, and at
another time it was behind it. This caused him considerable perplexity,
and, feeling convinced in his mind that the form of the planet's orbit
could not be circular, he was compelled to turn his attention to some
other closed curve, by which those inequalities of motion could be
explained.

After years of careful observation and study, Kepler arrived at the
conclusion that the form of the planet's orbit is an ellipse, and that
the Sun occupies one of the foci. He afterwards determined that the
orbits of all the planets are of an elliptical form.

Having discovered the true form of the planetary orbits, Kepler next
endeavoured to ascertain the cause which regulates the unequal motion
that a planet pursues in its path. He observed that when a planet
approached the Sun its motion was accelerated, and as it receded from
him its pace became slower.

This he explained in his next great discovery by proving that an
imaginary line, or radius-vector, extending from the centre of the Sun
to the centre of the planet 'describes equal areas in equal times.' When
near the Sun, or at perihelion, a planet traverses a larger portion of
its arc in the same period of time than it does when at the opposite
part of its orbit, or when at aphelion; but, as the areas of both are
equal, it follows that the planet does not always maintain the same rate
of speed, and that its velocity is greatest when nearest the Sun, and
least when most distant from him.

By the application of his first and second laws Kepler was able to
formulate a third law. He found that there existed a remarkable
relationship between the mean distances of the planets and the times in
which they complete their revolutions round the Sun, and discovered
'that the squares of the periodic times are to each in the same
proportion as the cubes of the mean distances.' The periodic time of a
planet having been ascertained, the square of the mean distance and the
mean distance itself can be obtained. It is by the application of this
law that the distances of the planets are usually calculated.

These discoveries are known as Kepler's Laws, and are usually classified
as follows:--

1. 'The orbit described by every planet is an ellipse, of which the
centre of the Sun occupies one of the foci.

2. 'Every planet moves round the Sun in a plane orbit, and the
radius-vector, or imaginary line joining the centre of the planet and
the centre of the Sun, describes equal areas in equal times.

3. 'The squares of the periodic times of any two planets are
proportional to the cubes of their mean distances from the Sun.'[1]

These remarkable discoveries do not embrace all the achievements by
which Kepler has immortalised his name, and earned for himself the proud
title of 'Legislator of the Heavens;' he predicted transits of Mercury
and Venus, made important discoveries in optics, and was the inventor of
the astronomical telescope.

GALILEO GALILEI, the famous Italian astronomer and philosopher, and the
contemporary of Kepler and of Milton, was born at Pisa on February 15,
1564.

His father, who traced his descent from an ancient Florentine family,
was desirous that his son should adopt the profession of medicine, and
with this intention he entered him as a student at the University of
Pisa. Galileo, however, soon discovered that the study of mathematics
and mechanical science possessed a greater attraction for his mind,
and, following his inclinations, he resolved to devote his energies to
acquiring proficiency in those subjects.

In 1583 his attention was attracted by the oscillation of a brass lamp
suspended from the ceiling of the cathedral at Pisa. Galileo was
impressed with the regularity of its motion as it swung backwards and
forwards, and was led to imagine that the pendulum movement might prove
a valuable method for the correct measurement of time. The practical
application of this idea he afterwards adopted in the construction of an
astronomical clock.

Having become proficient in mathematics, Galileo, whilst engaged in
studying the writings of Archimedes, wrote an essay on 'The Hydrostatic
Balance,' and composed a treatise on 'The Centre of Gravity in Solid
Bodies.' The reputation which he earned by these contributions to
science procured for him the appointment of Lecturer on Mathematics at
the University of Pisa. Galileo next directed his attention to the works
of Aristotle, and made no attempt to conceal the disfavour with which he
regarded many of the doctrines taught by the Greek philosopher; nor had
he any difficulty in exposing their inaccuracies. One of these, which
maintained that the heavier of two bodies descended to the earth with
the greater rapidity, he proved to be incorrect, and demonstrated by
experiment from the top of the tower at Pisa that, except for the
unequal resistance of the air, all bodies fell to the ground with the
same velocity.

As the chief expounder of the new philosophy, Galileo had to encounter
the prejudices of the followers of Aristotle, and of all those who
disliked any innovation or change in the established order of things.
The antagonism which existed between Galileo and his opponents, who were
both numerous and influential, was intensified by the bitterness and
sarcasm which he imparted into his controversies, and the attitude
assumed by his enemies at last became so threatening that he deemed it
prudent to resign the Chair of Mathematics in the University of Pisa.

In the following year he was appointed to a similar post at Padua, where
his fame attracted crowds of pupils from all parts of Europe.

In 1611 Galileo visited Rome. He was received with much distinction by
the different learned societies, and was enrolled a member of the
Lyncæan Academy. In two years after his visit to the capital he
published a work in which he declared his adhesion to the Copernican
theory, and openly avowed his disbelief in the astronomical facts
recorded in the Scriptures. Galileo maintained that the sacred writings
were not intended for the purpose of imparting scientific information,
and that it was impossible for men to ignore phenomena witnessed with
their eyes, or disregard conclusions arrived at by the exercise of their
reasoning powers.

The champions of orthodoxy having become alarmed, an appeal was made to
the ecclesiastical authorities to assist in suppressing this recent
astronomical heresy, and other obnoxious doctrines, the authorship of
which was ascribed to Galileo.

In 1615, Galileo was summoned before the Inquisition to reply to the
accusation of heresy. 'He was charged with maintaining the motion of the
Earth and the stability of the Sun; with teaching this doctrine to his
pupils; with corresponding on the subject with several German
mathematicians; and with having published it, and attempted to reconcile
it to Scripture in his letters to Mark Velser in 1612.'

These charges having been formally investigated by the Inquisition,
Cardinal Bellarmine was authorised to communicate with Galileo, and
inform him that unless he renounced the obnoxious doctrines, and
promised 'neither to teach, defend, or publish them in future,' it was
decreed that he should be committed to prison. Galileo appeared next day
before the Cardinal, and, without any hesitation, pledged himself that
for the future he would adhere to the pronouncement of the Inquisition.

Having, as they imagined, silenced Galileo, the Inquisition resolved to
condemn the entire Copernican system as heretical; and in order to
effectually accomplish this, besides condemning the writings of Galileo,
they inhibited Kepler's 'Epitome of the Copernican System,' and
Copernicus's own work, 'De Revolutionibus Orbium Celestium.'

Whether it was that Galileo regarded the Inquisition as a body whose
decrees were too absurd and unreasonable to be heeded, or that he
dreaded the consequences which might have followed had he remained
obstinate, we know that, notwithstanding the pledges which he gave, he
was soon afterwards engaged in controversial discussion on those
subjects which he promised not to mention again.

On the accession of his friend Cardinal Barberini to the pontifical
throne in 1623, under the title of Urban VIII., Galileo undertook a
journey to Rome to offer him his congratulations upon his elevation to
the papal chair. He was received by his Holiness with marked attention
and kindness, was granted several prolonged audiences, and had conferred
upon him several valuable gifts.

Notwithstanding the kindness of Pope Urban and the leniency with which
he was treated by the Inquisition, Galileo, having ignored his pledge,
published in 1632 a book, in dialogue form, in which three persons were
supposed to express their scientific opinions. The first upheld the
Copernican theory and the more recent philosophical views; the second
person adopted a neutral position, suggested doubts, and made remarks of
an amusing nature; the third individual, called Simplicio, was a
believer in Ptolemy and Aristotle, and based his arguments upon the
philosophy of the ancients.

As soon as this work became publicly known, the enemies of Galileo
persuaded the Pope that the third person held up to ridicule was
intended as a representation of himself--an individual regardless of
scientific truth, and firmly attached to the ideas and opinions
associated with the writings of antiquity.

Almost immediately after the publication of the 'Dialogues' Galileo was
summoned before the Inquisition, and, notwithstanding his feeble health
and the infirmities of advanced age, he was, after a long and tedious
trial, condemned to abjure by oath on his knees his scientific beliefs.

'The ceremony of Galileo's abjuration was one of exciting interest and
of awful formality. Clothed in the sackcloth of a repentant criminal,
the venerable sage fell upon his knees before the assembled cardinals,
and, laying his hand upon the Holy Evangelists, he invoked the Divine
aid in abjuring, and detesting, and vowing never again to teach the
doctrines of the Earth's motion and of the Sun's stability. He pledged
himself that he would nevermore, either in words or in writing,
propagate such heresies; and he swore that he would fulfil and observe
the penances which had been inflicted upon him.' 'At the conclusion of
this ceremony, in which he recited his abjuration word for word and then
signed it, he was conveyed, in conformity with his sentence, to the
prison of the Inquisition.'[2]

Galileo's sarcasm, and the bitterness which he imparted into his
controversies, were more the cause of his misfortunes than his
scientific beliefs. When he became involved in difficulties he did not
possess the moral courage to enable him to abide by the consequences of
his acts; nor did he care to become a martyr for the sake of science,
his submission to the Inquisition having probably saved him from a fate
similar to what befell Bruno. Though it would be impossible to justify
Galileo's want of faith in his dealings with the Inquisition, yet one
cannot help sympathising deeply with the aged philosopher, who, in this
painful episode of his life, was compelled to go through the form of
making a retractation of his beliefs under circumstances of a most
humiliating nature.

But the persecution of Galileo did not delay the progress of scientific
inquiry nor retard the advancement of the Copernican theory, which,
after the discovery by Newton of the law of gravitation, was universally
adopted as the true theory of the solar system.

Ferdinand, Duke of Tuscany, having exerted his influence with Pope Urban
on behalf of Galileo, he was, after a few days' incarceration, released
from prison, and permission was given him to reside at Siena, where he
remained for six months. He was afterwards allowed to return to his
villa at Arcetri, and, though regarded as a prisoner of the Inquisition,
was permitted to pursue his studies unmolested for the remainder of his
days.

Galileo died at Arcetri on January 8, 1642, when in the seventy-eighth
year of his age.

Though not the inventor, he was the first to construct a refracting
telescope and apply it to astronomical research. With this instrument
he made a number of important discoveries which tended to confirm his
belief in the truthfulness of the Copernican theory.

On directing his telescope to the Sun, he discovered movable spots on
his disc, and concluded from his observation of them that the orb
rotated on his axis in about twenty-eight days. He also ascertained that
the Moon's illumination is due to reflected sunlight, and that her
surface is diversified by mountains, valleys, and plains.

On the night of January 7, 1610, Galileo discovered the four moons of
Jupiter. This discovery may be regarded as one of his most brilliant
achievements with the telescope; and, notwithstanding the improvement in
construction and size of modern instruments, no other satellite was
discovered until near midnight on September 9, 1892, when Mr. E. E.
Barnard, with the splendid telescope of the Lick Observatory, added
'another gem to the diadem of Jupiter.'

The phases of Venus and Mars, the triple form of Saturn, and the
constitution of the Milky Way, which he found to consist of a countless
multitude of stars, were additional discoveries for our knowledge of
which we are indebted to Galileo and his telescope. Galileo made many
other important discoveries in mechanical and physical science. He
detected the law of falling bodies in their accelerated motion towards
the Earth, determined the parabolic law of projectiles, and
demonstrated that matter, even if invisible, possessed the property of
weight.

In these pages a short historical description is given of the progress
made in astronomical science from an early period to the time in which
Milton lived. The discoveries of Copernicus, Kepler, and Galileo had
raised it to a position of lofty eminence, though the law of
gravitation, which accounts for the form and permanency of the planetary
orbits, still remained undiscovered. Theories formerly obscure or
conjectural were either rejected or elucidated with accuracy and
precision, and the solar system, having the Sun as its centre, with his
attendant family of planets and their satellites revolving in majestic
orbits around him, presented an impressive spectacle of order, harmony,
and design.




CHAPTER II

ASTRONOMY IN THE SEVENTEENTH CENTURY


The seventeenth century embraces the most remarkable epoch in the whole
history of astronomy. It was during this period that those wonderful
discoveries were made which have been the means of raising astronomy to
the lofty position which it now occupies among the sciences. The
unrivalled genius and patient labours of the illustrious men whose names
stand out in such prominence on the written pages of the history of this
era have rendered it one of the most interesting and elevating of
studies. Though Copernicus lived in the preceding century, yet the names
of Tycho Brahé, Kepler, Galileo, and Newton, testify to the greatness of
the discoveries that were made during this period, which have surrounded
the memories of those men with a lustre of undying fame.

Foremost among astronomers of less conspicuous eminence who made
important discoveries in this century we find the name of Huygens.

CHRISTIAN HUYGENS was born at The Hague in 1629. He was the second son
of Constantine Huygens, an eminent diplomatist, and secretary to the
Prince of Orange. Huygens studied at Leyden and Breda, and became
highly distinguished as a geometrician and scientist. He made important
investigations relative to the figure of the Earth, and wrote a learned
treatise on the cause of gravity; he also determined with greater
accuracy investigations made by Galileo regarding the accelerated motion
of bodies when subjected to the influence of that force.

Huygens admitted that the planets and their satellites attracted each
other with a force varying according to the inverse ratio of the squares
of their distances, but rejected the mutual attraction of the molecules
of matter, believing that they possessed gravity towards a central point
only, to which they were attracted. This supposition was at variance
with the Newtonian theory, which, however, was universally regarded as
the correct one.

Huygens originated the theory by which it is believed that light is
produced by the undulatory vibration of the ether; he also discovered
polarization.

Up to this time the method adopted in the construction of clocks was not
capable of producing a mechanism which measured time with sufficient
accuracy to satisfy the requirements of astronomers. Huygens endeavoured
to supply this want, and applied his mechanical ingenuity in
constructing a clock that could be relied upon to keep accurate time.
Though the pendulum motion was first adopted by Galileo, he was unable
to arrange its mechanism so that it should keep up a continuous
movement. The oscillation of the pendulum ceased after a time, and a
fresh impulse had to be applied to set it in motion. Consequently,
Galileo's clock was of no service as a timekeeper.

Huygens overcame this difficulty by so arranging the mechanism of his
clock that the balance, instead of being horizontal, was directed
perpendicularly, and prolonged downwards to form a pendulum, the
oscillations of which regulated the downward motion of the weight. This
invention, which was highly applauded, proved to be of great service
everywhere, and was especially valuable for astronomical purposes.

Huygens next directed his attention to the construction of telescopes,
and displayed much skill in the grinding and polishing of lenses. He
made several instruments superior in power and accuracy to any that
existed previously, and with one of these made some remarkable
discoveries when observing the planet Saturn.

The telescopic appearance of Saturn is one of the most beautiful in the
heavens. The planet, surrounded by two brilliant rings, and accompanied
by eight attendant moons, surpasses all the other orbs of the firmament
as an object of interest and admiration. To the naked eye, Saturn is
visible as a star of the first magnitude, and was known to the ancients
as the most remote of the planets. Travelling in space at a distance of
nearly one thousand millions of miles from the Sun, the planet
accomplishes a revolution of its mighty orbit in twenty-nine and a half
years.

Galileo was the first astronomer who directed a telescope to Saturn. He
observed that the planet presented a triform appearance, and that on
each side of the central globe there were two objects, in close contact
with it, which caused it to assume an ovoid shape. After further
observation, Galileo perceived that the lateral bodies gradually
decreased in size, until they became invisible. At the expiration of a
certain period of time they reappeared, and were observed to go through
a certain cycle of changes. By the application of increased telescopic
power it was discovered that the appendages were not of a rounded form,
but appeared as two small crescents, having their concave surfaces
directed towards the planet and their extremities in contact with it,
resembling the manner in which the handles are attached to a cup.

These objects were observed to go through a series of periodic changes.
After having become invisible, they reappeared as two luminous straight
bands, projecting from each side of the planet; during the next seven or
eight years they gradually opened out, and assumed a crescentic form;
they afterwards began to contract, and on the expiration of a similar
period, during which time they gradually decreased in size, they again
became invisible. It was perceived that the appendages completed a cycle
of their changes in about fifteen years.

In 1656, Huygens, with a telescope constructed by himself, was enabled
to solve the enigma which for so many years baffled the efforts of the
ablest astronomers. He announced his discovery in the form of a Latin
cryptograph which, when deciphered, read as follows:--

'Annulo cingitur, tenui plano, nusquam cohaerente, ad eclipticam
inclinatio.'

'The planet is surrounded by a slender flat ring everywhere distinct
from its surface, and inclined to the ecliptic.'

Huygens perceived the shadow of the ring thrown on the planet, and was
able to account in a satisfactory manner for all the phenomena observed
in connection with its variable appearance.

The true form of the ring is circular, but by us it is seen
foreshortened; consequently, when the Earth is above or below its plane,
it appears of an elliptical shape. When the position of the planet is
such that the plane of the ring passes through the Sun, the edge of the
ring only is illumined, and then it becomes invisible for a short
period. In the same manner, when the plane of the ring passes through
the Earth, the illumined edge of the ring is not of sufficient magnitude
to appear visible, but as the enlightened side of the plane becomes more
inclined towards the Earth, the ring comes again into view. When the
plane of the ring passes between the Earth and the Sun, the unillumined
side of the ring is turned towards the Earth, and during the time it
remains in this position it is invisible.

Huygens discovered the sixth satellite of Saturn (Titan), and also the
Great Nebula in Orion.

JOHANN HEVELIUS, a celebrated Prussian astronomer, was born at Dantzig
in 1611, and died in that city in 1687. He was a man of wealth, and
erected an observatory at his residence, where, for a period of forty
years, he carried out a series of astronomical observations.

He constructed a chart of the stars, and in order to complete his work,
formed nine new constellations in those spaces in the celestial vault
which were previously un-named. They are known by the names
Camelopardus, Canes Venatici, Coma Bernices, Lacerta, Leo Minor, Lynx,
Monoceros, Sextans, and Vulpecula. He also executed a chart of the
Moon's surface, wrote a description of the lunar spots, and discovered
the Libration of the Moon in Longitude.

On May 30, 1661, Hevelius observed a transit of Mercury, a description
of which he published, and included with it Horrox's treatise on the
first-recorded transit of Venus. This work, after having passed through
several hands, became the property of Hevelius, who was capable of
appreciating its merits. The manuscript was sent to him by Huygens, and
in acknowledging it he writes: 'How greatly does my Mercury exult in the
joyous prospect that he may shortly fold within his arms Horrox's long
looked-for and beloved Venus! He renders you unfeigned thanks that by
your permission this much-desired union is about to be celebrated, and
that the writer is able, with your concurrence, to introduce them both
together to the public.'

Hevelius made numerous researches on comets, and suggested that the
form of their paths might be a parabola.

GIOVANNI DOMENICO CASSINI was born at Perinaldo, near Nice, in 1625. He
studied at Genoa and Bologna, and was afterwards appointed to the Chair
of Astronomy at the latter University. He was a man of high scientific
attainments, and made many important astronomical discoveries.

In 1671 he became Director of the Royal Observatory at Paris, and
devoted a long life to trying and difficult observations, which in his
later years deprived him of his eyesight.

In 1644 Cassini proved beyond doubt that Jupiter rotated on his axis,
and also assigned his period of rotation with considerable accuracy. He
published tables of the planet's satellites, and determined their
motions from observations of their eclipses. He ascertained the periods
of rotation of Venus and Mars; executed a chart of the lunar surface,
and observed an occultation of Jupiter by the Moon.

Cassini discovered the dual nature of Saturn's ring, having perceived
that instead of one there are two concentric rings separated by a dark
space. He also discovered four of the planet's satellites--viz. Japetus,
Rhea, Dione, and Tethys. He made a near approximation to the solar
parallax by means of researches on the parallax of Mars, and
investigated some irregularities of the Moon's motion. Cassini
discovered the belts of Jupiter, and also the Zodiacal Light, and
established the coincidence of the nodes of the lunar equator and orbit.

JAQUES CASSINI, son of Giovanni, was born at Paris in 1677. He followed
in his father's footsteps, and wrote several treatises on astronomical
subjects. He investigated the period of the rotation of Venus on her
axis, and upheld the results arrived at by his father, which were
afterwards confirmed by observations made by Schroeter. Cassini made
some valuable researches with regard to the proper motion of the stars,
and demonstrated that their change of position on the celestial vault
was real, and not caused by a displacement of the ecliptic. He attempted
to ascertain the apparent diameter of Sirius, and made observations with
regard to the visibility of the stars. The Cassini family produced
several generations of eminent astronomers, whose discoveries and
investigations were of much value in advancing the science of astronomy.

OLAUS ROEMER, an eminent Danish astronomer, was born at Copenhagen
September 25, 1644. When Picard, a French astronomer, visited Denmark in
1671, for the purpose of ascertaining the exact position of
'Uranienburg,' the site of Tycho Brahé's observatory, he made the
acquaintance of Roemer, who was engaged in studying mathematics and
astronomy under Erasmus Bartolinus. Having perceived that the young man
was gifted with no ordinary degree of talent, he secured his services to
assist him in his observations, and, on the conclusion of his labours,
Picard was so much impressed with the ability displayed by Roemer, that
he invited him to accompany him to France. This invitation he accepted,
and took up his residence in the French capital, where he continued to
prosecute his astronomical studies.

In 1675 Roemer communicated to the Academy of Sciences a paper, in which
he announced his discovery of the progressive transmission of light. It
was believed that light travelled instantaneously, but Roemer was able
to demonstrate the inaccuracy of this conclusion, and determined that
light travels through space with a measurable velocity.

By diligently observing the eclipses of Jupiter's satellites, Roemer
perceived that sometimes they occurred before, and sometimes after their
predicted times. This irregularity, he discovered, depended upon the
position of the Earth with regard to Jupiter. When the Earth, in
traversing her orbit, moved round to the opposite side of the Sun,
thereby bringing Jupiter into conjunction, an eclipse occurred sixteen
minutes twenty-six seconds later than it did when Jupiter was in
opposition or nearest to the Earth. As there existed an impression that
light travelled instantaneously, it was believed that an eclipse
occurred at the moment it was perceived in the telescope. This, however,
was not so. Roemer, after a long series of observations, concluded that
the discrepancies were due to the fact that light travels with a
measurable velocity, and that it requires a greater length of time,
upwards of sixteen minutes, to traverse the additional distance--the
diameter of the Earth's orbit--which intervenes between the Earth and
Jupiter, when the planet is in conjunction, as compared with the
distance between the Earth and Jupiter, when the latter is in
opposition. This discovery of Roemer's was the means of enabling the
velocity of light to be ascertained, which, according to recent
calculations, is about 187,000 miles a second. As an acknowledgment of
the importance of his communication, Roemer was awarded a seat in the
Academy, and apartments were assigned to him at the Royal Observatory,
where he carried on his astronomical studies.

In 1681 Roemer returned to Denmark, and was appointed Professor of
Mathematics in the University of Copenhagen; he was also entrusted with
the care of the city observatory--a duty which his reputation as an
astronomer eminently qualified him to undertake. The transit
instrument--a mechanism of much importance to astronomers--was invented
by Roemer in 1690; it consists of a telescope fixed to a horizontal
axis, and adjusted so as to revolve in the plane of the meridian. It is
employed in observing the passage of the heavenly bodies across the
observer's meridian. To note accurately by means of the astronomical
clock the exact instant of time at which a celestial body crosses the
centre of the field of view is the essential part of a transit
observation. Small transit instruments are employed for taking the time
and for regulating the observatory clock, but large instruments are
used for delicate and exact observations of Right Ascensions and
Declinations of stars of different magnitudes. Meridian, and altitude
and azimuth circles, are important astronomical appliances, which owe
their existence to the inventive skill of this distinguished astronomer.

Roemer resided for many years at the observatory in the city of
Copenhagen, where he pursued his astronomical studies until the time of
his death, which occurred in 1710. He meritoriously attempted to
determine the parallax of the fixed stars; and it is said that the
astronomical calculations and observations which he left behind him were
so voluminous as to equal in number those made by Tycho Brahé, nearly
all of which perished in a great conflagration that destroyed the
observatory and a large portion of the city of Copenhagen in 1728.

Among other astronomers of this century whose names deserve recording
were Descartes and Gassendi, whose mathematical researches in their
application to astronomy were of much value; Fabricius, Torricelli, and
Maraldi, who by their observations and investigations added many facts
to the general knowledge of the science; and Bayer, to whom belongs the
distinction of having constructed the first star-atlas.

In our own country during this period astronomy was cultivated by a few
enthusiastic men, who devoted their time and talents to promoting the
advancement of the science. It, however, received no recognition as a
subject of study at any of the Universities, and no public observatory
existed in Great Britain.

Though it was not until towards the close of the century that the
attention of all Europe was directed to England in admiration of the
discoveries of the illustrious Newton, yet astronomy had its humble
votaries, and chief among those was a young clergyman of the name of
Horrox.

JEREMIAH HORROX was born at Toxteth, near Liverpool, in 1619--close on
three centuries ago. Little is known of his family. His parents have
been described as persons who occupied a humble position in life, but,
as they were able to give their son a classical education which fitted
him for one of the learned professions, it is probable they were not so
obscure as they have been represented to be.

Having received his early education at Toxteth, Horrox afterwards
proceeded to Cambridge, and was entered as a student at Emmanuel College
on May 18, 1632, when in his fourteenth year.

At the University he devoted himself to the study of classics,
especially Latin, which in those days was the language adopted by men of
learning, when engaged in writing works of a philosophical and
scientific character.

After having remained at Cambridge for three years, Horrox returned to
his native county, and was appointed curate of Hoole, a place about
eight miles distant from Preston. Hoole is described as a narrow
low-lying strip of land consisting largely of moss, and almost converted
into an island by the waters of Martin Mere on the south, and the Ribble
on the north; and, though doubtless an open and favourable situation for
astronomical observation, it could not have been attractive as a place
of residence. Yet it was here on November 24, 1639, that Horrox made his
famous observation of the first recorded transit of Venus, an occurrence
with which his name will be for ever associated.

It was while at Cambridge that Horrox first turned his attention to the
study of astronomy. His love of the sublime, and the captivating
influence exerted on his mind by the contemplation of the heavenly
bodies, induced him to adopt astronomy as a pursuit congenial to his
tastes, and capable of exercising his highest mental powers. Having this
object in view, he applied himself with much earnestness to the study of
mathematics; he had, however, to rely mainly upon his own exertions, for
at that time no branch of physical or mathematical science was taught at
Cambridge, and consequently he obtained no professional instruction.

It was so also with astronomy, which, as a science, was scarcely known
in this country; no regular record of astronomical observations was kept
by any individual observer, and no public observatory existed in England
or in France.

The disadvantages and obstacles which Horrox had to encounter may be
best described by quoting his own words. He writes: 'There were many
hindrances. The abstruse nature of the study, my inexperience and want
of means dispirited me. I was much pained not to have any one to whom I
could look for guidance, or indeed for the sympathy of companionship in
my endeavours, and I was assailed by the languor and weariness which are
inseparable from every great undertaking. What then was to be done? I
could not make the pursuit an easy one, much less increase my fortune,
and least of all imbue others with a love for astronomy; and yet to
complain of philosophy on account of its difficulties would be foolish
and unworthy. I determined, therefore, that the tediousness of study
should be overcome by industry; my poverty--failing a better method--by
patience; and that instead of a master I would use astronomical books.
Armed with these weapons I would contend successfully; and, having heard
of others acquiring knowledge without greater help, I would blush that
any one should be able to do more than I, always remembering that word
of Virgil's--

    Totidem nobis animaeque manusque.

Having heard much praise bestowed upon the works of Lansberg, a Flemish
astronomer, Horrox thought it would be to his advantage to procure a
copy of his writings. This he succeeded in obtaining after some
difficulty, and devoted a considerable time to calculating Ephemerides,
based upon the Lansberg Tables, but after making a number of
computations he discovered that they were unreliable and inaccurate.

In the year 1636 Horrox made the acquaintance of William Crabtree, a
devoted astronomer, who lived at Broughton, a suburb of Manchester. A
close friendship soon existed between the two men, and they carried on
an active correspondence about matters relating to the science which
they both loved so well.

Crabtree, who was an unbeliever in Lansberg, urged Horrox to discard the
Flemish astronomer's works, and devote his talents to the study of Tycho
Brahé and Kepler. This advice led Horrox to make a more rigorous
examination of the Lansberg Tables, and after comparing them with the
observations made by Crabtree, which coincided with his own, he resolved
to renounce them. Acting on the advice of his friend, Horrox directed
his attention to the writings of Kepler. The youthful astronomer soon
realised their value, and was charmed with the accuracy of observation
and inductive reasoning displayed in the elucidation of those general
laws which constituted a new era in the history of astronomy.

The Rudolphine Tables, which were the astronomical calculations
commenced by Tycho Brahé, and completed by Kepler, were regarded by
Horrox as much superior to those of Lansberg; but it occurred to him
that they might be improved by changing some of the numbers, and yet
retaining the hypotheses. To this task he applied himself with much
earnestness and assiduity, and after close application and laborious
study he accomplished the arduous undertaking of bringing those tables
to a high state of perfection.

In his investigation of the Lunar theory, Horrox outstripped all his
predecessors, and Sir Isaac Newton distinctly affirms he was the first
to discover that the Moon's motion round the Earth is in the form of an
ellipse with the centre in the lower focus. Besides having made this
discovery, Horrox was able to explain the causes of the inequalities of
the Moon's motion, which render the exact computation of her elements so
difficult.

The Annual Equation, an irregularity discovered by Tycho Brahé, which is
produced by the increase and decrease of the Sun's disturbing force as
the Earth approaches or recedes from him in her orbit, had its value
first assigned by Horrox. This he calculated to be eleven minutes
sixteen seconds, which is within four seconds of what it has since been
proved to be by the most recent observations.

The Evection, an irregular motion of the Moon discovered by Ptolemy,
whereby her mean longitude is increased or diminished, was explained by
Horrox as depending upon the libratory motion of the apsides, and the
change which takes place in the eccentricity of the lunar orbit.

These discoveries were made by Horrox before he attained the age of
twenty years, and if his reputation had alone rested upon them his name
would have been honourably associated with those who have attained to
the highest eminence in astronomy.

Another achievement which adds lustre to Horrox's name consists in his
detection of the inequality in the mean motions of Jupiter and Saturn.

He also directed his attention to the study of cometary bodies, and
arrived at certain conclusions with regard to the nature of their
movements. At first, he believed like Kepler that comets were projected
in straight lines from the Sun; this supposition having been upheld on
account of the great elongation of their orbits. He next perceived that
their velocity increased as they approached the Sun, and decreased as
they receded from him. Afterwards he says, 'They move in an elliptic
figure or near it,' and finally he arrived at the conclusion that
'comets move in elliptical orbits, being carried round the Sun with a
velocity which is probably variable.' This theory has been verified by
numerous observations, and is now generally accepted by astronomers.

Horrox also made a series of observations on the tides. He notified the
extent of their rise and fall at different periods, and investigated
other phenomena associated with their ebb and flow. After having
continued his observations for some time, he wrote to his friend
Crabtree, and informed him that he had perceived many interesting
details which had not been previously described, and he hoped to be
able to arrive at some important conclusions with regard to their nature
and cause. Unfortunately, Horrox's writings on this subject, along with
many other important papers, have been lost or destroyed. We are
therefore ignorant of the result of his researches, which were the first
undertaken by any person for the purpose of scientific inquiry.

From his study of the Lansberg and Rudolphine Tables, Horrox arrived at
the conclusion that a transit of Venus would occur on November 24, 1639.
This transit was for some unaccountable reason overlooked by Kepler, who
predicted one in 1631, and the next not until 1761. The transit of 1631
was not visible in Europe.

We are indebted to Horrox for a description of the transit of 1639--the
first that was ever observed of which there is any record; and were it
not for the accuracy of his calculations, the occurrence of the
phenomenon would have been unperceived, and no history of the
conjunction would have been handed down to posterity. As soon as Horrox
had assured himself of the time when the transit would take place, he
wrote to Crabtree to inform him of the date, and asked him to make
observations with his telescope, and especially to examine the diameter
of the planet, which he thought had been over-estimated. He also
requested him to write to Dr. Foster of Cambridge, and inform him of the
expected event, as it was desirable that the transit should be observed
from several places in consequence of the possibility of failure, owing
to an overcast sky. His letter is dated October 26, 1639. He says: 'My
reason for now writing is to advise you of a remarkable conjunction of
the Sun and Venus on the 24th of November, when there will be a transit.
As such a thing has not happened for many years past, and will not occur
again in this century, I earnestly entreat you to watch attentively with
your telescope in order to observe it as well as you can.

'Notice particularly the diameter of Venus, which is stated by Kepler to
be seven minutes, and by Lansberg to be eleven, but which I believe to
be scarcely greater than one minute.'

In describing the method which he adopted for observing the transit,
Horrox writes as follows: 'Having attentively examined Venus with my
instrument, I described on a sheet of paper a circle, whose diameter was
nearly equal to six inches--the narrowness of the apartment not
permitting me conveniently to use a larger size. I divided the
circumference of this circle into 360 degrees in the usual manner, and
its diameter into thirty equal parts, which gives about as many minutes
as are equivalent to the Sun's apparent diameter. Each of these thirty
parts was again divided into four equal portions, making in all one
hundred and twenty; and these, if necessary, may be more minutely
subdivided. The rest I left to ocular computation, which, in such small
sections, is quite as certain as any mechanical division. Suppose,
then, each of these thirty parts to be divided into sixty seconds,
according to the practice of astronomers. When the time of the
observation approached, I retired to my apartment, and, having closed
the windows against the light, I directed my telescope--previously
adjusted to a focus--through the aperture towards the Sun, and received
his rays at right angles upon the paper already mentioned. The Sun's
image exactly filled the circle, and I watched carefully and unceasingly
for any dark body that might enter upon the disc of light.

'Although the corrected computation of Venus' motions which I had before
prepared, and on the accuracy of which I implicitly relied, forbade me
to expect anything before three o'clock in the afternoon of the 24th,
yet since, according to the calculations of most astronomers, the
conjunction should take place sooner--by some even on the 23rd--I was
unwilling to depend entirely on my own opinion, which was not
sufficiently confirmed, lest by too much self-confidence I might
endanger the observation. Anxiously intent, therefore, on the
undertaking through the greater part of the 23rd, and on the whole of
the 24th, I omitted no available opportunity of observing her ingress. I
watched carefully on the 24th from sunrise to nine o'clock, and from a
little before ten until noon, and at one in the afternoon, being called
away in the intervals by business of the highest importance, which for
these ornamental pursuits I could not with propriety neglect.[3] But
during all this time I saw nothing in the Sun except a small and common
spot, consisting as it were of three points at a distance from the
centre towards the left, which I noticed on the preceding and following
days. This evidently had nothing to do with Venus. About fifteen minutes
past three in the afternoon, when I was again at liberty to continue my
labours, the clouds, as if by divine interposition, were entirely
dispersed, and I was once more invited to the grateful task of repeating
my observations. I then beheld a most agreeable spectacle--the object of
my sanguine wishes; a spot of unusual magnitude and of a perfectly
circular shape, which had already fully entered upon the Sun's disc on
the left, so that the limbs of the Sun and Venus precisely coincided,
forming an angle of contact. Not doubting that this was really the
shadow of the planet, I immediately applied myself sedulously to observe
it.

'In the first place, with respect to the inclination, the line of the
diameter of the circle being perpendicular to the horizon, although its
plane was somewhat inclined on account of the Sun's altitude, I found
that the shadow of Venus at the aforesaid hour--namely, fifteen minutes
past three--had entered the Sun's disc about 62° 30´, certainly between
60° and 65°, from the top towards the right. This was the appearance in
the dark apartment; therefore, out of doors, beneath the open sky,
according to the laws of optics, the contrary would be the case, and
Venus would be below the centre of the Sun, distant 62° 30´ from the
lower limbs or the nadir, as the Arabians term it. The inclination
remained to all appearances the same until sunset, when the observation
was concluded.

'In the second place, the distance between the centres of Venus and the
Sun I found by three observations to be as follows:--

          The Hour.          | Distance of the Centres.
                             |
At 3·15 by the clock         |        14´ 24´´
 " 3·35      "               |        13´ 30´´
 " 3·45      "               |        13´  0´´
 " 3·50 the apparent sunset. |

The true setting being 3·45, and the apparent about 5 minutes later, the
difference being caused by refraction. The clock therefore was
sufficiently correct.

'In the third place I found after careful and repeated observation that
the diameter of Venus, as her shadow was depicted on the paper, was
larger indeed than the thirtieth part of the solar diameter, though not
more so than the sixth, or at the utmost the fifth of such a part.
Therefore let the diameter of the Sun be to the diameter of Venus as 30´
to 1´ 12´´. Certainly her diameter never equalled 1´ 30´´, scarcely
perhaps 1´ 20´´, and this was evident as well when the planet was near
the Sun's limb as when far distant from it.

[Illustration: VENUS ON THE SUN'S DISC.]

'This observation was made in an obscure village where I have long been
in the habit of observing, about fifteen miles to the north of
Liverpool, the latitude of which I believe to be 53° 20´, although by
common maps it is stated at 54° 12´, therefore the latitude of the
village will be 53° 35´, and longitude of both 22° 30´ from the
Fortunate Islands, now called the Canaries. This is 14° 15´ to the west
of Uraniburg in Denmark, the longitude of which is stated by Brahé, a
native of the place, to be 36° 45´ from these islands.

'This is all I could observe respecting this celebrated conjunction
during the short time the Sun remained in the horizon: for although
Venus continued on his disc for several hours, she was not visible to me
longer than half an hour on account of his so quickly setting.
Nevertheless, all the observations which could possibly be made in so
short a time I was enabled by Divine Providence to complete so
effectually that I could scarcely have wished for a more extended
period. The inclination was the only point upon which I failed to attain
the utmost precision; for, owing to the rapid motion of the Sun it was
difficult to observe with certainty to a single degree, and I frankly
confess that I neither did nor could ascertain it. But all the rest is
sufficiently accurate, and as exact as I could desire.'

Besides having ascertained that the diameter of Venus subtends an angle
not much greater than one minute of arc, Horrox reduced the horizontal
solar parallax from fifty-seven seconds as stated by Kepler to fourteen
seconds, a calculation within one and a half second of the value
assigned to it by Halley sixty years after. He also reduced the Sun's
semi-diameter.

Crabtree, to whom Horrox refers as 'his most esteemed friend and a
person who has few superiors in mathematical learning,' made
preparations to observe the transit similar to those already described.
But the day was unfavourable, dark clouds obscured the sky and rendered
the Sun invisible. Crabtree was in despair, and relinquished all hope of
being able to witness the conjunction. However, just before sunset there
was a break in the clouds, and the Sun shone brilliantly for a short
interval. Crabtree at once seized his opportunity, and to his intense
delight observed the planet fully entered upon the Sun's disc. Instead
of proceeding to take observations, he was so overcome with emotion at
the sight of the phenomenon, that he continued to gaze upon it with rapt
attention, nor did he recover his self-possession until the clouds again
hid from his view the setting Sun.[4]

Crabtree's observation of the transit was, however, not a fruitless one.
He drew from memory a diagram showing the exact position of Venus on the
Sun's disc, which corresponded in every respect with Horrox's
observation; he also estimated the diameter of the planet to be 7/200
that of the Sun, which when calculated gives one minute three seconds;
Horrox having found it to be one minute twelve seconds. This transit of
Venus is remarkable as having been the first ever observed of which
there is any record, and for this we are indebted to the genius of
Horrox, who by a series of calculations, displaying a wonderfully
accurate knowledge of mathematics, was enabled to predict the occurrence
of the phenomenon on the very day, and almost at the hour it appeared,
and of which he and his friend Crabtree were the only observers.

Having thought it desirable to write an account of the transit, Horrox
prepared an elegant Latin treatise, entitled 'Venus in Sole
Visa'--'Venus seen in the Sun;' but not knowing what steps to take with
regard to its publication, he requested Crabtree to communicate with his
bookseller and obtain his advice on the matter.

In the meantime Horrox returned to Toxteth, and arranged to fulfil a
long-promised visit to Crabtree, which he looked forward to with much
pleasure, as it would afford him an opportunity of discussing with his
friend many matters of interest to both. This visit was frustrated in a
manner altogether unexpected. For we read that Horrox was seized with a
sudden and severe illness, the nature of which is not known, and that
his death occurred on the day previous to that of his intended visit to
his friend at Broughton. He expired on January 3, 1641, when in the 23rd
year of his age.

His death was a great grief to Crabtree, who, in one of his letters,
describes it as 'an irreparable loss:' and it is believed that he only
survived him a few years.[5] Of the papers left by Horrox, only a few
have been preserved, and these were discovered in Crabtree's house after
his death. Among them was his treatise on the transit of Venus which,
with other papers, was purchased by Dr. Worthington, Fellow of Emmanuel
College, Cambridge, a man of learning, who was capable of appreciating
their value. Ultimately, the treatise fell into the possession of
Hevelius, a celebrated German astronomer, who published it along with a
dissertation of his own, describing a transit of Mercury.

Horrox did not live to see any of his writings published, nor was any
monument erected to his memory until nearly two hundred years after his
death. But his name, though long forgotten except by astronomers, is now
engraved on marble in Westminster Abbey. Had his life been spared, it
would have been difficult to foretell to what eminence and fame he might
have risen, or what further discoveries his genius might have enabled
him to make. Few among English astronomers will hesitate to rank him
next with the illustrious Newton, and all will agree with Herschel, who
called him 'the pride and the boast of British Astronomy.'

WILLIAM GASCOIGNE was born in 1612, in the parish of Rothwell, in the
county of York, and afterwards resided at Middleton, near Leeds.

He was a man of an inventive turn of mind, and possessed good abilities,
which he devoted to improving the methods of telescopic observation.

At an early age he was occupied in observing celestial objects, making
researches in optics, and acquiring a proficient knowledge of astronomy.

Among his acquaintances were Crabtree and Horrox, with whom he carried
on a correspondence on matters appertaining to their favourite study.

The measurement of small angles was found at all times to be one of the
greatest difficulties which astronomers had to contend with. Tycho Brahé
was so misled by his measurements of the apparent diameters of the Sun
and Moon, that he concluded a total eclipse of the Sun was impossible.

Gascoigne overcame this difficulty by his invention of the micrometer.
This instrument, when applied to a telescope, was found to be of great
service in the correct measurement of minute angles and distances, and
was the means of greatly advancing the progress of practical astronomy
in the seventeenth century. A micrometer consists of a short tube,
across the opening of which are stretched two parallel wires; these
being intersected at right angles by a third. The wires are moved to or
from each other by delicately constructed screws, to which they are
attached. Each revolution, or part of a revolution, of a screw indicates
the distance by which the wires are moved.

This apparatus, when placed in the focus of a lens, gives very accurate
measurements of the diameters of celestial objects. It was successfully
used by Gascoigne in determining the apparent diameters of the Sun,
Moon, and several of the planets, and the mutual distances of the stars
which form the Pleiades.

Crabtree, after having paid Gascoigne a visit in 1639, describes in a
letter to Horrox the impression created on his mind by the micrometer.
He writes: 'The first thing Mr. Gascoigne showed me was a large
telescope, amplified and adorned with new inventions of his own, whereby
he can take the diameters of the Sun or Moon, or any small angle in the
heavens or upon the earth, most exactly through the glass to a second.'

The micrometer is now regarded as an indispensable appliance in the
observatory; the use of a spider web reticule instead of wire having
improved its efficiency. Gascoigne was one of the earliest astronomers
who recognised the value of the Keplerian telescope for observational
purposes, and Sherburn affirms that he was the first to construct an
instrument of this description having two convex lenses. Whether this be
true or not, it is certain that he applied the micrometer to the
telescope, and was the first to use telescopic sights, by means of which
he was able to fix the optical axis of his telescope, and ascertain by
observation the apparent positions of the heavenly bodies.

Crabtree, in a letter to Gascoigne, says: 'Could I purchase it with
travel, or procure it with gold, I would not be without a telescope for
observing small angles in the heavens; or want the use of your device of
a glass in a cane upon the movable ruler of your sextant, as I remember
for helping to the exact point of the Sun's rays.'

It was not known until the beginning of the eighteenth century that
Gascoigne had invented and used telescopic sights for the purpose of
making accurate astronomical observations. The accidental discovery of
some documents which contained a description of his appliances was the
means by which this became known.

Townley states that Gascoigne had completed a treatise on optics, which
was ready for publication, but that no trace of the manuscript could be
discovered after his death. Having embraced the Royalist cause, William
Gascoigne joined the forces of Charles I., and fell in the battle of
Marston Moor on July 2, 1644.

The early death of this young and remarkably clever man was a severe
blow to the science of astronomy in England.

The invention of logarithms, by Baron Napier, of Merchistoun, was found
to be of inestimable value to astronomers in facilitating and
abbreviating the methods of astronomical calculation.

By the use of logarithms, arithmetical computations which necessitated
laborious application for several months could with ease be completed in
as many days. It was remarked by Laplace that this invention was the
means of doubling the life of an astronomer, besides enabling him to
avoid errors and the tediousness associated with long and abstruse
calculations.

THOMAS HARRIOT, an eminent mathematician, and an assiduous astronomer,
made some valuable observations of the comet of 1607. He was one of the
earliest observers who made use of the telescope, and it was claimed on
his behalf that he discovered Jupiter's satellites, and the spots on the
Sun, independently of Galileo. Other astronomers have been desirous of
sharing this honour, but it has been conclusively proved that Galileo
was the first who made those discoveries.

The investigations of Norwood and Gilbert, the mechanical genius of
Hooke, and the patient researches of Flamsteed--the first Astronomer
Royal--were of much value in perfecting many details associated with the
study of astronomy.

The Royal Observatory at Greenwich was founded in 1675. The building was
erected under a warrant from Charles II. It announces the desire of the
Sovereign to build a small observatory in the park at Greenwich, 'in
order to the finding out of the longitude for perfecting the art of
navigation and astronomy.' This action on the part of the King may be
regarded as the first public acknowledgment of the usefulness of
astronomy for national purposes.

Since its erection, the observatory has been presided over by a
succession of talented men, who have raised it to a position of eminence
and usefulness unsurpassed by any similar institution in this or any
other country. The well-known names of Flamsteed, Halley, Bradley, and
Airy, testify to the valuable services rendered by those past directors
of the Greenwich Observatory in the cause of astronomical science.

If we take a general survey of the science of astronomy as it existed
from 1608 to 1674--a period that embraced the time in which Milton
lived--we shall find that it was still compassed by ignorance,
superstition, and mystery. Astrology was zealously cultivated; most
persons of rank and position had their nativity or horoscope cast, and
the belief in the ruling of the planets, and their influence on human
and terrestrial affairs, was through long usage firmly established in
the public mind. Indeed, at this time, astronomy was regarded as a
handmaid to astrology; for, with the aid of astronomical calculation,
the professors of this occult science were enabled to predict the
positions of the planets, and by this means practised their art with an
apparent degree of truthfulness.

Although over one hundred years had elapsed since the death of
Copernicus, his theory of the solar system did not find many supporters,
and the old forms of astronomical belief still retained their hold on
the minds of the majority of philosophic thinkers. This can be partly
accounted for, as many of the Ptolemaic doctrines were at first
associated with the Copernican theory, nor was it until a later period
that they were eliminated from the system.

Though Copernicus deserved the credit of having transferred the centre
of our system from the Earth to the Sun, yet his theory was imperfect in
its details, and contained many inaccuracies. He believed that the
planets could only move round the Sun in circular paths, nor was he
capable of conceiving of any other form of orbit in which they could
perform their revolutions. He was therefore compelled to retain the use
of cycles and epicycles, in order to account for irregularities in the
uniformly circular motions of those bodies.

We are indebted to the genius of Kepler for having placed the Copernican
system upon a sure and irremovable basis, and for having raised
astronomy to the position of a true physical science. By his discovery
that the planets travel round the Sun in elliptical orbits, he was
enabled to abolish cycles and epicycles, which created such confusion
and entanglement in the system, and to explain many apparent
irregularities of motion by ascribing to the Sun his true position with
regard to the motions of the planets.

After the death of Kepler, which occurred in 1630, the most eminent
supporter of the Copernican theory was the illustrious Galileo, whose
belief in its accuracy and truthfulness was confirmed by his own
discoveries.

Five of the planets were known at this time--viz. Mercury, Venus, Mars,
Jupiter, and Saturn; the latter, which revolves in its orbit at a
profound distance from the Sun, formed what at that time was believed to
be the boundary of the planetary system. The distance of the Earth from
the Sun was approximately known, and the orb was observed to rotate on
his axis.

It was also ascertained that the Moon shone by reflected light, and that
her surface was varied by inequalities resembling those of our Earth.
The elliptical form of her orbit had been discovered by Horrox, and her
elements were computed with a certain degree of accuracy.

The cloudy luminosity of the Milky Way had been resolved into a
multitude of separate stars, disclosing the immensity of the stellar
universe.

The crescent form of the planet Venus, the satellites of Jupiter and of
Saturn, and the progressive motion and measurement of light, had also
been discovered. Observations were made of transits of Mercury and
Venus, and refracting and reflecting telescopes were invented.

The law of universal gravitation, a power which retains the Earth and
planets in their orbits, causing them year after year to describe with
unerring regularity their oval paths round the Sun, was not known at
this time. Though Newton was born in 1642, he did not disclose the
results of his philosophic investigations until 1687--thirteen years
after the death of Milton--when, in the 'Principia,' he announced his
discovery of the great law of universal gravitation.

Kepler, though he discovered the laws of planetary motion, was unable to
determine the motive force which guided and retained those bodies in
their orbits. It was reserved for the genius of Newton to solve this
wonderful problem. This great philosopher was able to prove 'that every
particle of matter in the universe attracts every other particle with a
force proportioned to the mass of the attracting body, and inversely as
the square of the distance between them.' Newton was capable of
demonstrating that the force which guides and retains the Earth and
planets in their orbits resides in the Sun, and by the application of
this law of gravitation he was able to explain the motions of all
celestial bodies entering into the structure of the solar system.

This discovery may be regarded as the crowning point of the science of
astronomy, for, upon the unfailing energy of this mysterious power
depend the order and stability of the universe, extending as it does to
all material bodies existing in space, guiding, controlling, and
retaining them in their several paths and orbits, whether it be a tiny
meteor, a circling planet, or a mighty sun.

The nature of cometary bodies and the laws which govern their motions
were at this time still enshrouded in mystery, and when one of those
erratic wanderers made its appearance in the sky it was beheld by the
majority of mankind with feelings of awe and superstitious dread, and
regarded as a harbinger of evil and disaster, the precursor of war, of
famine, or the overthrow of an empire.

Newton, however, was able to divest those bodies of the mystery with
which they were surrounded by proving that any conic section may be
described about the Sun, consistent with the law of gravitation, and
that comets, notwithstanding the eccentricity of their orbits, obey the
laws of planetary motion.

Beyond the confines of our solar system, little was known of the
magnitude and extent of the sidereal universe which occupies the
infinitude of space by which we are surrounded. The stars were
recognised as self-luminous bodies, inconceivably remote, and although
they excited the curiosity of observers, and conjectures were made as to
their origin, yet no conclusive opinions were arrived at with regard to
their nature and constitution, and except that they were regarded as
glittering points of light which illumine the firmament, all else
appertaining to them remained an unravelled mystery. Even Copernicus had
no notion of a universe of stars.

Galileo, by his discovery that the galaxy consists of a multitude of
separate stars too remote to be defined by ordinary vision, demonstrated
how vast are the dimensions of the starry heavens, and on what a
stupendous scale the universe is constructed. But at this time it had
not occurred to astronomers, nor was it known until many years after,
that the stars are suns which shine with a splendour resembling that of
our Sun, and in many instances surpassing it. It was not until this
truth became known that the glories of the sidereal heavens were fully
comprehended, and their magnificence revealed. It was then ascertained
that the minute points of light which crowd the fields of our largest
telescopes, in their aggregations forming systems, clusters, galaxies,
and universes of stars, are shining orbs of light, among the countless
multitudes of which our Sun may be numbered as one.




CHAPTER III

MILTON'S ASTRONOMICAL KNOWLEDGE


It would be reasonable to imagine that Milton's knowledge of astronomy
was comprehensive and accurate, and superior to that possessed by most
scientific men of his age. His scholarly attainments, his familiarity
with ancient history and philosophy, his profound learning, and the
universality of his general knowledge, would lead one to conclude that
the science which treats of the mechanism of the heavens, and especially
the observational part of it--which at all times has been a source of
inspiration to poets of every degree of excellence--was to him a study
of absorbing interest, and one calculated to make a deep impression upon
his devoutly poetical mind. The serious character of Milton's verse, and
the reverent manner in which celestial incidents and objects are
described in it, impress one with the belief that his contemplation of
the heavens, and of the orbs that roll and shine in the firmament
overhead, afforded him much enjoyment and meditative delight. For no
poet, in ancient or in modern times, has introduced into his writings
with such frequency, or with such pleasing effect, so many passages
descriptive of the beauty and grandeur of the heavens. No other poet,
by the creative effort of his imagination, has soared to such a height;
nor has he ever been excelled in his descriptions of the celestial orbs,
and of the beautiful phenomena associated with their different motions.

In his minor poems, which were composed during his residence at Horton,
a charming rural retreat in Buckinghamshire, where the freshness and
varied beauty of the landscape and the attractive aspects of the
midnight sky were ever before him, we find enchanting descriptions of
celestial objects, and especially of those orbs which, by their
brilliancy and lustre, have always commanded the admiration of mankind.

For example, in 'L'Allegro' there are the following lines:--

    Right against the eastern gate
    Where the great Sun begins his state,
    Robed in flames and amber light,
    The clouds in thousand liveries dight;

and in 'Il Penseroso'--

    To behold the wandering Moon,
    Riding near her highest noon,
    Like one that had been led astray
    Through the heaven's wide pathless way,
    And oft as if her head she bowed,
    Stooping through a fleecy cloud.

In the happy choice of his theme, and by the comprehensive manner in
which he has treated it, Milton has been enabled by his poetic genius to
give to the world in his 'Paradise Lost' a poem which, for sublimity of
thought, loftiness of imagination, and beauty of expression in metrical
verse, is unsurpassed in any language.

It is, however, our intention to deal only with those passages in the
poem in which allusion is made to the heavenly bodies, and to incidents
and occurrences associated with astronomical phenomena. In the
exposition and illustration of these it has been considered desirable to
adopt the following general classification:--

1. To ascertain the extent of Milton's astronomical knowledge.

2. To describe the starry heavens and the celestial objects mentioned in
'Paradise Lost.'

3. To exemplify the use which Milton has made of astronomy in the
exercise of his imaginative and descriptive powers.

In the earlier half of the seventeenth century the Ptolemaic theory--by
which it was believed that the Earth was the immovable centre of the
universe, and that round it all the heavenly bodies completed a diurnal
revolution--still retained its ascendency over the minds of men of
learning and science, and all the doctrines associated with this ancient
astronomical creed were still religiously upheld by the educated classes
among the peoples inhabiting the different civilised regions of the
globe. The Copernican theory--by which the Sun is assigned the central
position in our system, with the Earth and planets revolving in orbits
round him--obtained the support of a few persons of advanced views and
high scientific attainments, but its doctrines had not yet seriously
threatened the supremacy of the older system. Though upwards of one
hundred years had elapsed since the death of Copernicus, yet the
doctrines associated with the system of which he was the founder were
but very tardily adopted up to this time. There were several reasons
which accounted for this. The Copernican system was at first imperfect
in its details, and included several of the Ptolemaic, doctrines which
rendered it less intelligible, and retarded its acceptance by persons
who would otherwise have been inclined to adopt it. Copernicus believed
that the planets travelled round the Sun in circular paths. This
necessitated the retention of cycles and epicycles, which gave rise to
much confusion; nor was it until Kepler made his great discovery of the
ellipticity of the planetary orbits that they were eliminated from the
system.

As the Ptolemaic system of the universe held complete sway over the
minds of men for upwards of twenty centuries, it was difficult to
persuade many persons to renounce the astronomical beliefs to which they
were so firmly attached, in favour of those of any other system; so that
the overthrow of this venerable theory required a lengthened period of
time for its accomplishment.

It was thus in his earlier years, when Milton devoted his time to the
study of literature and philosophy, which he read extensively when
pursuing his academic career at Christ's College, Cambridge, and
afterwards at Horton, where he spent several years in acquiring a more
proficient knowledge of the literary, scientific, and philosophical
writings of the age, that he found the beliefs associated with the
Ptolemaic theory adopted without doubt or hesitation by the numerous
authors whose works he perused. His knowledge of Italian enabled him to
become familiar with Dante--one of his favourite authors, whose poetical
writings were deeply read by him, and who, in the elaboration of his
poem, the 'Divina Commedia,' included the entire Ptolemaic cosmology.

In England the Copernican theory had few supporters, and the majority of
those who represented the intellect and learning of the country still
retained their adherence to the old form of astronomical belief. We
therefore find that Milton followed the traditional way of thinking by
adopting the views associated with the Ptolemaic theory.

According to the Ptolemaic system, the Earth was regarded as the
immovable centre of the universe, and surrounding it were ten
crystalline spheres, or heavens, arranged in concentric circles, the
larger spheres enclosing the smaller ones; and within those was situated
the cosmos, or mundane universe, usually described as 'the Heavens and
the Earth.' To each of the first seven spheres there was attached a
heavenly body, which was carried round the Earth by the revolution of
the crystalline.

1st sphere: that of the Moon.

2nd sphere: that of the planet Mercury.

3rd sphere: that of the planet Venus.

4th sphere: that of the Sun; regarded as a planet.

5th sphere: that of the planet Mars.

6th sphere: that of the planet Jupiter.

7th sphere: that of the planet Saturn.

8th sphere: that of the fixed stars.

[Illustration: FIG. 1]

The eighth sphere included all the fixed stars, and was called the
firmament, because it was believed to impart steadiness to the inner
spheres, and, by its diurnal revolution, to carry them round the Earth,
causing the change of day and night.

The separate motions of the spheres, revolving with different
velocities, and at different angles to each other, accounted for the
astronomical phenomena associated with the orbs attached to each.
According to Ptolemy's scheme, the eighth sphere formed the outermost
boundary of the universe; but later astronomers added to this system two
other spheres--a _ninth_, called the _Crystalline_, which caused
Precession of the Equinoxes; and a _tenth_, called the _Primum Mobile_,
or First Moved, which brought about the alternation of day and night, by
carrying all the other spheres round the Earth once in every twenty-four
hours. The Primum Mobile enclosed, as if in a shell, all the other
spheres, in which was included the created universe, and, although of
vast dimensions, its conception did not overwhelm the mind in the same
manner that the effort to comprehend infinitude does.

Beyond this last sphere there was believed to exist a boundless,
uncircumscribed region, of immeasurable extent, called the Empyrean, or
Heaven of Heavens, the incorruptible abode of the Deity, the place of
eternal mysteries, which the comprehension of man was unable to fathom,
and of which it was impossible for his mind to form any conception. Such
were the imaginative beliefs upon which this ancient astronomical theory
was founded, that for a period of upwards of two thousand years held
undisputed sway over the minds of men, and exercised during that time a
predominating influence upon the imagination, thoughts, and conceptions
of all those who devoted themselves to literature, science, and art. Of
the truthfulness of this assertion there is ample evidence in the
poetical, philosophical, and historical writings of ancient authors,
whose ideas and conceptions regarding the created universe were limited
and circumscribed by this form of astronomical belief. In the works of
more recent writers we find that it continued to assert its influence;
and among our English poets, from Chaucer down to Shakespeare, there are
numerous references to the natural phenomena associated with this
system, and most frequently expressed by poetical allusions to 'the
music of the spheres.'

The ideas associated with the Ptolemaic theory were gratifying to the
pride and vanity of man, who could regard with complacency the paramount
importance of the globe which he inhabited, and of which he was the
absolute ruler, fixed in the centre of the universe, and surrounded by
ten revolving spheres, that carried along with them in their circuit all
other celestial bodies--Sun, Moon, and stars, which would appear to have
been created for his delectation, and for the purpose of ministering to
his requirements. But when the Copernican theory became better
understood, and especially after the discovery of the law of universal
gravitation, this venerable system of the universe, based upon a pile of
unreasonable and false hypotheses, after an existence of over twenty
centuries, sank into oblivion, and was no more heard of.

Milton's Ptolemaism is apparent in some of his shorter pieces, and also
in his minor poems, 'Arcades' and 'Comus.' His 'Ode on the Nativity' is
written in conformity with this belief, and the expression,

    Ring out ye crystal spheres,

indicates a poetical allusion to this theory. But as Milton grew older
his Ptolemaism became greatly modified, and there are good reasons for
believing that in his latter years he renounced it entirely in favour of
Copernicanism. When on his continental tour in 1638, he made the
acquaintance of eminent men who held views different from those with
which he was familiar; and in his interview with Galileo at Arcetri, the
aged astronomer may have impressed upon his mind the superiority of the
Copernican theory, in accounting for the occurrence of celestial
phenomena, as compared with the Ptolemaic.

On his return to England from the Continent, Milton took up his
residence in London, and lived in apartments in a house in St. Bride's
Churchyard. Having no regular vocation, and not wishing to be dependent
upon his father, he undertook the education of his two nephews, John and
Edward Phillips, aged nine and ten years respectively. From St. Bride's
Churchyard he removed to a larger house in Aldersgate, where he received
as pupils the sons of some of his most intimate acquaintances. In the
list of subjects which Milton selected for the purpose of imparting
instruction to those youths he included astronomy and mathematics,
which formed part of the curriculum of this educational establishment.
The text-book from which he taught his nephews and other pupils
astronomy was called 'De Sphæra Mundi,' a work written by Joannes
Sacrobasco (John Holywood) in the thirteenth century. This book was an
epitome of Ptolemy's 'Almagest,' and therefore entirely Ptolemaic in its
teaching. It enjoyed great popularity during the Middle Ages, and is
reported to have gone through as many as forty editions.

The selection of astronomy as one of the subjects in which Milton
instructed his pupils affords us evidence that he must have devoted
considerable time and attention to acquiring a knowledge of the facts
and details associated with the study of the science. In the attainment
of this he had to depend upon his own exertions and the assistance
derived from astronomical books; for at this time astronomy received no
recognition as a branch of study at any of the universities; and in
Britain the science attracted less attention than on the Continent,
where the genius of Kepler and Galileo elevated it to a position of
national importance.

We shall find as we proceed that Milton's knowledge of astronomy was
comprehensive and accurate; that he was familiar with the astronomical
reasons by which many natural phenomena which occur around us can be
explained; and that he understood many of the details of the science
which are unknown to ordinary observers of the heavens.

It is remarkable how largely astronomy enters into the composition of
'Paradise Lost,' and we doubt if any author could have written such a
poem without possessing a knowledge of the heavens and of the celestial
orbs such as can only be attained by a proficient and intimate
acquaintance with this science.

The arguments in favour of or against the Ptolemaic and Copernican
theories were well known to Milton, even as regards their minute
details; and in Book viii. he introduces a scientific discussion based
upon the respective merits of those theories. The configuration of the
celestial and terrestrial spheres, and the great circles by which they
are circumscribed, he also knew. The causes which bring about the change
of the seasons; the obliquity of the ecliptic; the zodiacal
constellations through which the Sun travels, and the periods of the
year in which he occupies them, are embraced in Milton's knowledge of
the science of astronomy. The motions of the Earth, including the
Precession of the Equinoxes; the number and distinctive appearances of
the planets, their direct and retrograde courses, and their satellites,
are also described by him. The constellations, and their relative
positions on the celestial sphere; the principal stars, star-groups, and
clusters, and the Galaxy, testify to Milton's knowledge of astronomy,
and to the use which he has made of the science in the elaboration of
his poem.

The names of fourteen of the constellations are mentioned in 'Paradise
Lost.' These, when arranged alphabetically, read as follows:--

Andromeda, Aries, Astrea, Centaurus, Cancer, Capricornus, Gemini, Leo,
Libra, Ophiuchus, Orion, Scorpio, Taurus, and Virgo. Milton's allusions
to the zodiacal constellations are chiefly associated with his
description of the Sun's path in the heavens; but with the celestial
sign Libra (the _Scales_) he has introduced a lofty and poetical
conception of the means by which the Creator made known His will when
there arose a contention between Gabriel and Satan on his discovery in
Paradise.

    The Eternal, to prevent such horrid fray,
    Hung forth in Heaven his golden scales, yet seen
    Betwixt Astrea[6] and the Scorpion sign,
    Wherein all things created first he weighed,
    The pendulous round Earth with balanced air
    In counterpoise, now ponders all events,
    Battles and realms. In these he put two weights,
    The sequel each of parting and of fight:
    The latter quick up flew, and kicked the beam.--iv. 996-1004.

Orion, the finest constellation in the heavens, did not escape Milton's
observation, and there is one allusion to it in his poem. It arrives on
the meridian in winter, where it is conspicuous as a brilliant
assemblage of stars, and represents an armed giant, or hunter, holding a
massive club in his right hand, and having a shield of lion's hide on
his left arm. A triple-gemmed belt encircles his waist, from which is
suspended a glittering sword, tipped with a bright star. The two
brilliants Betelgeux and Bellatrix form the giant's shoulders, and the
bright star Rigel marks the position of his advanced foot. The rising of
Orion was believed to be accompanied by stormy and tempestuous weather.
Milton alludes to this in the following lines:--

          When with fierce winds Orion armed
    Hath vexed the Red Sea coast, whose waves o'erthrew
    Busiris and his Memphian chivalry.--i. 305-7.

Andromeda is described as being borne by Aries, and in 'Ophiuchus huge'
Milton locates a comet which extends the whole length of the
constellation. It is evident that Milton possessed a precise knowledge
of the configuration and size of the constellations, and of the
positions which they occupy relatively to each other on the celestial
sphere.

Though Milton was conversant with the Copernican theory, and entertained
a conviction of its accuracy and truthfulness, and doubtless recognised
the superiority of this system, which, besides conveying to the mind a
nobler conception of the universe and of the solar system--though it
diminished the importance of the Earth as a member of it--was capable of
explaining the occurrence of celestial phenomena in a manner more
satisfactory than could be arrived at by the Ptolemaic theory.
Notwithstanding this, he selected the Ptolemaic cosmology as the
scientific basis upon which he constructed his 'Paradise Lost,' and in
its elaboration adhered with marked fidelity to this system. There were
many reasons why Milton, in the composition of an imaginative poem,
should have chosen the Ptolemaic system of the universe rather than the
Copernican. This form of astronomical belief was adopted by all the
authors whose works he perused and studied in his younger days,
including his favourite poet, Dante; and his own poetic imaginings, as
indicated by his early poems, were in harmony with the doctrines of this
astronomical creed, a long acquaintance with which had, without doubt,
influenced his mind in its favour. This system of revolving spheres,
with the steadfast Earth at its centre, and the whole enclosed by the
Primum Mobile, constituted a more attractive and picturesque object for
poetic description than the simple and uncircumscribed arrangement of
the universe expressed by the Copernican theory. It also afforded him an
opportunity of localising those regions of space in which the chief
incidents in his poem are described--viz. HEAVEN, or THE EMPYREAN,
CHAOS, HELL, and the MUNDANE UNIVERSE. Milton's Ptolemaism, with its
adjuncts, may be understood by the following:

All that portion of space above the newly created universe, and beyond
the Primum Mobile, was known as HEAVEN, or THE EMPYREAN--a region of
light, of glory, and of happiness; the dwelling-place of the Deity, Who,
though omnipresent, here visibly revealed Himself to all the multitude
of angels whom He created, and who surrounded his throne in adoration
and worship.

Underneath the universe there existed a vast region of similar
dimensions to the Empyrean, called CHAOS, which was occupied by the
embryo elements of matter, that with incessant turmoil and confusion
warred with each other for supremacy--a wild abyss--

    The womb of Nature and perhaps her grave.--ii. 911.

The lower portion of this region was divided off from the remainder, and
embraced the locality known as HELL--the place of torment, where the
rebellious angels were driven and shut in after their expulsion from
Heaven.

    As far removed from God and light of Heaven
    As from the centre thrice to the utmost pole.--i. 73-74.

The NEW UNIVERSE, which included the Earth and all the orbs of the
firmament known as the Starry Heavens, was created out of Chaos, and
hung, as if suspended by a golden chain, from the Empyrean above; and
although its magnitude and dimensions were inconceivable, yet, according
to the Ptolemaic theory, it was enclosed by the tenth sphere or Primum
Mobile.

By this partitioning of space Milton was able to contrive a system which
fulfilled the requirements of his great poem.

The annexed diagram explains the relative positions of the different
regions into which space was divided.

Though there are traces of Copernicanism found in 'Paradise Lost,' yet
Milton has very faithfully adhered to the Ptolemaic mechanism and
nomenclature throughout his poem.

In his description of the Creation, the Earth is formed first, then the
Sun, followed by the Moon, and afterwards the stars, all of which are
described as being in motion round the Earth. Allusion is also made to
this ancient system in several prominent passages, and in the following
lines there is a distinct reference to the various revolving spheres.

[Illustration: FIG. 2]

    They pass the planets seven, and pass the fixed,
    And that crystalline sphere whose balance weighs
    The trepidation talked, and that first moved.--iii. 481-83.

The seven planetary spheres are first mentioned; then the eighth sphere,
or that of the fixed stars; then the ninth, or crystalline, which was
believed to cause a shaking, or trepidation, to account for certain
irregularities in the motions of the stars; and, lastly, the tenth
sphere, or Primum Mobile, called the 'first moved' because it set the
other spheres in motion.

To an uninstructed observer, the apparent motion of the heavenly bodies
round the Earth would naturally lead him to conclude that, of the two
theories, the Ptolemaic was the correct one. We therefore find that
Milton adopted the system most in accord with the knowledge and
intelligence possessed by the persons portrayed by him in his poem; and
in describing the natural phenomena witnessed in the heavens by our
first parents, he adheres to the doctrines of the Ptolemaic system, as
being most in harmony with the simple and primitive conceptions of those
created beings.

To their upward gaze, the orbs of heaven appeared to be in ceaseless
motion; the solid Earth, upon which they stood, was alone immovable and
at rest. Day after day they observed the Sun pursue his steadfast course
with unerring regularity: his rising in the east, accompanied by the
rosy hues of morn; his meridian splendour, and his sinking in the west,
tinting in colours of purple and gold inimitable the fleecy clouds
floating in the azure sky, as he bids farewell for a time to scenes of
life and happiness, rejoicing in the light and warmth of his
all-cheering beams. With the advent of night they beheld the Moon, now
increasing, now waning, pursue her irregular path, also to disappear in
the west; whilst, like the bands of an army marshalled in loose array,
the constellations of glittering stars, with stately motion, traversed
their nocturnal arcs, circling the pole of the heavens.

By referring to Book viii., 15-175, we find an account of an interesting
scientific discussion, or conversation, between Adam and Raphael
regarding the merits of the Ptolemaic and Copernican systems, and of the
relative importance and size of the heavenly bodies. By it we are
afforded an opportunity of learning how accurate and precise a knowledge
Milton possessed of both theories, and in what clear and perspicuous
language he expresses his arguments in favour of or against the
doctrines associated with each.

We may, with good reason, regard the views expressed by Adam as
representing Milton's own opinions, which were in conformity with the
Copernican theory; and in the Angel's reply, though of an undecided
character, we are able to perceive how aptly Milton describes the
erroneous conclusions upon which the Ptolemaic theory was based.

In this scientific discussion, it would seem rather strange that Adam,
the first of men, should have been capable of such philosophic
reasoning, propounding, as if by intuition, a theory upon which was
founded a system that had not been discovered until many centuries after
the time that astronomy became a science. By attributing to Adam such a
degree of intelligence and wisdom, the poet has taken a liberty which
enabled him to carry on this discussion in a manner befitting the
importance of the subject.

In the following lines Adam expresses to his Angel-guest, in forcible
and convincing language, his reasons in support of the Copernican
theory:--

    When I behold this goodly frame, this World,
    Of Heaven and Earth consisting, and compute
    Their magnitudes--this Earth, a spot, a grain,
    An atom, with the Firmament compared
    And all her numbered stars, that seem to roll
    Spaces incomprehensible (for such
    Their distance argues, and their swift return
    Diurnal) merely to officiate light
    Round this opacous Earth, this punctual spot,
    One day and night, in all her vast survey
    Useless besides--reasoning, I oft admire,
    How Nature, wise and frugal could commit
    Such disproportions, with superfluous hand
    So many nobler bodies to create,
    Greater so manifold, to this one use,
    For aught appears, and on their Orbs impose
    Such restless revolution day by day
    Repeated, while the sedentary Earth,
    That better might with far less compass move,
    Served by more noble than herself, attains
    Her end without least motion, and receives,
    As tribute, such a sumless journey brought
    Of incorporeal speed, her warmth and light;
    Speed, to describe whose swiftness number fails.--viii. 15-38.

We are enabled to perceive that Milton had formed a correct conception
of the magnitude and proportions of the universe, and also of the
relative size and importance of the Earth, which he describes as 'a
spot, a grain, an atom,' when compared with the surrounding heavens. He
expresses his surprise that all the stars of the firmament, whose
distances are so remote, and whose dimensions so greatly exceed those of
this globe, should in their diurnal revolution have 'such a sumless
journey of incorporeal speed imposed upon them' merely to officiate
light to the Earth, 'this punctual spot;' and reasoning, wonders how
Nature, wise and frugal in her ways, should commit such disproportions,
by adopting means so great to accomplish a result so small, when motion
imparted to the sedentary Earth would with greater ease produce the same
effect.

The inconceivable velocity with which it would be necessary for those
orbs to travel in order to accomplish a daily revolution round the Earth
might be described as almost spiritual, and beyond the power of
calculation by numbers.

The Angel, after listening to Adam's argument, expresses approval of his
desire to obtain knowledge, but answers him dubiously, and at the same
time criticises in a severe and adverse manner the Ptolemaic theory.

    To ask or search I blame thee not; for Heaven
    Is as the Book of God before thee set,
    Wherein to read his wondrous works, and learn
    His seasons, hours, or days, or months, or years.
    This to attain, whether Heaven move or Earth,
    Imports not, if thou reckon right; the rest
    From Man or Angel the Great Architect
    Did wisely to conceal, and not divulge
    His secrets, to be scanned by them who ought
    Rather admire. Or, if they list to try
    Conjecture, he his fabric of the Heavens
    Hath left to their disputes, perhaps to move
    His laughter at their quaint opinions wide
    Hereafter, when they come to model Heaven,
    And calculate the stars; how they will wield
    The mighty frame; how build, unbuild, contrive
    To save appearances; how gird the Sphere
    With Centric and Eccentric scribbled o'er
    Cycle and Epicycle, Orb in Orb.--viii. 66-84.

When, with the advancement of science, astronomical observations were
made with greater accuracy, it was discovered that uniformity of motion
was not always maintained by those bodies which were believed to move in
circles round the Earth. It was observed that the Sun, when on one side
of his orbit, had an accelerated motion, as compared with the speed at
which he travelled when on the other side. The planets, also, appeared
to move with irregularity: sometimes a planet was observed to advance,
then become stationary, and afterwards affect a retrograde movement.
Those inequalities of motion could not be explained by means of the
revolution of crystalline spheres alone, but were accounted for by
imagining the existence of a small circle, or epicycle, whose centre
corresponded with a fixed point in the larger circle, or eccentric, as
it was called. This small circle revolved on its axis when carried round
with the larger one, and round it the planet also revolved, which when
situated in its outer portion would have a forward, and when in its
inner portion a retrograde, motion.

The theory of eccentrics and epicycles was sufficient for a time to
account for the inequalities of motion already described, and by this
means the Ptolemaic system was enabled to retain its ascendency for a
longer period than it otherwise would have done. But more recent
discoveries brought to light discrepancies and difficulties which were
explained away by adding epicycle to epicycle. This created a most
complicated entanglement, and hastened the downfall of a system which,
after an existence of many centuries, sank into oblivion, and is now
remembered as a belief of bygone ages.

The devices which the upholders of this system were compelled to adopt,
in order 'to save appearances,' with 'centric and eccentric,' cycle and
epicycle, 'orb in orb,' are in this manner appropriately described by
Milton, as indicating the confusion arising from a theory based upon
false hypotheses.

Continuing his reply, the Angel says:--

    Already by thy reasoning this I guess,
    Who art to lead thy offspring, and supposest
    That bodies bright and greater should not serve
    The less not bright, nor Heaven such journies run,
    Earth sitting still, when she alone receives
    The benefit. Consider, first, that great
    Or bright infers not excellence. The Earth,
    Though, in comparison of Heaven, so small,
    Nor glistering, may of solid good contain
    More plenty than the Sun that barren shines,
    Whose virtue on itself works no effect,
    But in the fruitful Earth; there first received,
    His beams, inactive else, their vigour find,
    Yet not to Earth are those bright luminaries
    Officious, but to thee, Earth's habitant.
    And, for the Heaven's wide circuit, let it speak
    The Maker's high magnificence, who built
    So spacious, and his line stretched out so far,
    That Man may know he dwells not in his own--
    An edifice too large for him to fill,
    Lodged in a small partition; and the rest
    Ordained for uses to his Lord best known,
    The swiftness of those Circles attribute,
    Though numberless, to his Omnipotence,
    That to corporeal substances could add
    Speed almost spiritual. Me thou think'st not slow,
    Who since the morning-hour set out from Heaven
    Where God resides, and ere midday arrived
    In Eden--distance inexpressible
    By numbers that have name. But this I urge,
    Admitting motion in the Heavens, to show
    Invalid that which thee to doubt it moved;
    Not that I so affirm, though so it seem
    To thee who hast thy dwelling here on Earth.
    God, to remove his ways from human sense,
    Placed Heaven from Earth so far, that earthly sight,
    If it presume, might err in things too high,
    And no advantage gain.--viii. 85-122.

Notwithstanding the Angel's severe criticism of the Ptolemaic system, he
does not unreservedly support the conclusions arrived at by Adam, but
endeavours to show that his reasoning may not be altogether correct. He
questions the validity of his argument that bodies of greater size and
brightness should not serve the smaller, though not bright, and that
heaven should move, while the Earth remained at rest. He argues that
great or bright infers not excellence, and that the Earth, though small,
may contain more virtue than the Sun, that 'barren shines,' whose beams
create no beneficial effect, except when directed on the fruitful
Earth. He reminds Adam that those bright luminaries minister not to the
Earth, but to himself, 'Earth's habitant,' and directs his attention to
the magnificence and extent of the surrounding universe, of which he
occupies but a small portion. The diurnal swiftness of the orbs that
move round the Earth he attributes to God's omnipotence, that to
material bodies 'could add speed almost spiritual.'

The Angel, after alluding to his rapid flight through space, suggests
that God placed heaven so far from Earth that man might not presume to
inquire into things which it would be of no advantage for him to know.
He then suddenly changes to the Copernican system, which he lucidly
describes in the following lines:--

                              What if the Sun
    Be centre to the World, and other stars
    By his attractive virtue and their own
    Incited, dance about him various rounds?
    Their wandering course, now high, now low, then hid,
    Progressive, retrograde, or standing still,
    In six thou seest; and what if, seventh to these
    The planet Earth, so steadfast though she seem,
    Insensibly three different motions move?
    Which else to several spheres thou must ascribe,
    Moved contrary with thwart obliquities,
    Or save the Sun his labour, and that swift
    Nocturnal and diurnal rhomb supposed
    Invisible else above all stars, the wheel
    Of day and night; which needs not thy belief,
    If Earth, industrious of herself, fetch day
    Travelling east, and with her part averse
    From the Sun's beam meet night, her other part
    Still luminous by his ray. What if that light,
    Sent from her through the wide transpicuous air,
    To the terrestrial Moon be as a star,
    Enlightening her by day, as she by night
    This Earth--reciprocal, if land be there,
    Fields and inhabitants? Her spots thou seest
    As clouds, and clouds may rain, and rain produce
    Fruits in her softened soil, for some to eat
    Allotted there; and other Suns, perhaps,
    With their attendant Moons, thou wilt descry,
    Communicating male and female light--
    Which two great sexes animate the World,
    Stored in each orb perhaps with some that live.
    For such vast room in Nature unpossessed
    By living soul, desert and desolate,
    Only to shine, yet scarce to contribute
    Each orb a glimpse of light, conveyed so far
    Down to this habitable, which returns
    Light back to them, is obvious to dispute.--viii. 122-58.

The Copernican theory, which is less complicated and more easily
understood than the Ptolemaic, is described by Milton with accuracy and
methodical skill.

The Sun having been assigned that central position in the system which
his magnitude and importance claim as his due, the planets circling in
orbits around him have their motions described in a manner indicative of
the precise knowledge which Milton acquired of this theory. At this time
the law of gravitation was unknown, and, although the ellipticity of the
orbits of the planets had been discovered by Kepler, the nature of the
motive force which guided and retained them in their paths still
remained a mystery. It was believed that the planets were whirled round
the Sun, as if by the action of magnetic fibres; a mutual attractive
influence having been supposed to exist between them and the orb,
similar to that of the opposite poles of magnets.

Milton alludes to this theory in the following lines:--

                            They, as they move
    Their starry dance in numbers that compute
    Days, months, and years, towards his all-cheering lamp
    Turn swift their various motions, or are turned
    By his magnetic beam.--iii. 579-83.

An important advance upon this theory was made by Horrox, who, in his
study of celestial dynamics, attributed the curvilineal motion of the
planets to the influence of two forces, one projective, the other
attractive. He illustrated this by observing the path described by a
stone when thrown obliquely into the air. He perceived that its motion
was governed by the impulse imparted to it by the hand, and also by the
attractive force of the Earth. Under these two influences, the stone
describes a graceful curve, and in its descent falls at the same angle
at which it rose. Hence arises the general law: 'When two spheres are
mutually attracted, and if not prevented by foreign influences, their
straight paths are deflected into curves concave to each other, and
corresponding with one of the sections of a cone, according to the
velocity of the revolving body. If the velocity with which the revolving
body is impelled be equal to what it would acquire by falling through
half the radius of a circle described from the centre of deflection, its
orbit will be circular; but if it be less than that quantity, its path
becomes elliptical.'

Newton afterwards embraced this law in his great principle of
gravitation, and demonstrated that the force which guides and retains
the Earth and planets in their orbits resides in the Sun. By the orb's
attractive influence a planet, after having received its first impulse,
is deflected from its original straight path, and bent towards that
luminary, and by the combined action of the projective and attractive
forces is made to describe an orbit which, if elliptical, has one of its
foci occupied by the Sun. So evenly balanced are those two forces, that
one is unable to gain any permanent ascendency over the other, and
consequently the planet traverses its orbit with unerring regularity,
and, if undisturbed by external influences, will continue in its path
for all time.

Milton describes the position of the planets in the sky as--

    Now high, now low, then hid;

and their motions--

    Progressive, retrograde, or standing still.

It is evident that Milton was familiar with the apparently irregular
paths pursued by the planets when observed from the Earth. He knew of
their stationary points, and also the backward loopings traced out by
them on the surface of the sphere.

If observed from the Sun, all the planets would be seen to follow their
true paths round that body; their motion would invariably lie in the
same direction, and any variation in their speed as they approached
perihelion or aphelion would be real. But the planets, when observed
from the Earth, which is itself in motion, appear to move irregularly.
Sometimes they remain stationary for a brief period, and, instead of
progressing onward, affect a retrograde movement. This irregularity of
motion is only apparent, and can be explained as a result of the
combined motions of the Earth and planets, which are travelling together
round the Sun with different velocities, and in orbits of unequal
magnitude.

In his allusion to the Copernican system the 'planet' 'Earth' is
described by Milton as seventh. This is not strictly accurate, as only
five planets were known--viz. Mercury, Venus, Mars, Jupiter, and Saturn;
but to make up the number Milton has included the Moon, which may be
regarded as the Earth's planet.

The three motions ascribed to the Earth are--(1) The diurnal rotation on
her axis; (2) her annual revolution round the Sun; (3) Precession of the
Equinoxes.

The rotation of the Earth on her axis may be likened to the spinning
motion of a top, and is the cause of the alternation of day and night.
This rotatory motion is sustained with such exact precision that, during
the past 2,000 years, it has been impossible to detect the minutest
difference in the time in which the Earth accomplishes a revolution on
her axis, and therefore the length of the sidereal day, which is 3
minutes 56 seconds shorter than the mean solar day, is invariable. In
this motion of the Earth we have a time-measuring unit which may be
regarded as absolutely correct.

The Earth completes a revolution of her orbit in 365-1/4 days. In this
period of time she accomplishes a journey of 580 millions of miles,
travelling at the average rate of 66,000 miles an hour. The change of
the seasons, and the lengthening and shortening of the day, are natural
phenomena, which occur as a consequence of the Earth's annual revolution
round the Sun. Precession is a retrograde or westerly motion of the
equinoctial points, caused by the attraction of the Sun, Moon, and
planets on the spheroidal figure of the Earth. By this movement the
poles of the Earth are made to describe a circular path in that part of
the heavens to which they point; so that, after the lapse of many years,
the star which is known as the Pole Star will not occupy the position
indicated by its name, but will be situated at a considerable distance
from the pole. These motions, Milton says, unless attributed to the
Earth, must be ascribed to several spheres crossing and thwarting each
other obliquely; but the Earth, by rotating from west to east, will of
herself fetch day, her other half, averted from the Sun's rays, being
enveloped in night. Thus saving the Sun his labour, and the 'primum
mobile,' 'that swift nocturnal and diurnal rhomb,' which carried all the
lower spheres along with it, and brought about the change of day and
night.

Milton's allusion to the occurrence of natural phenomena in the Moon
similar to those which happen on the Earth is in keeping with the
opinions entertained regarding our satellite, Galileo having imagined
that he discovered with his telescope continents and seas on the lunar
surface, which led to the belief that the Moon was the abode of
intelligent life.

    ... and other suns, perhaps,
    With their attendant moons, thou wilt descry
    Communicating male and female light.--viii. 148-50.

Milton in these lines refers to Jupiter and Saturn, and their
satellites, which had been recently discovered; those of the former by
Galileo, and four of those of the latter by Cassini. The existence of
male and female light was an idea entertained by the ancients, and which
is mentioned by Pliny. The Sun was regarded as a masculine star, and the
Moon as feminine; the light emanating from each being similarly
distinguished, and possessing different properties.

Milton supposes that, as the Earth receives light from the stars, she
returns light back to them. But in his time little was known about the
stars, nor was it ascertained how distant they are.

The Angel, in bringing to a conclusion his conversation with Adam, deems
it unadvisable to vouchsafe him a decisive reply to his inquiry
regarding the motions of celestial bodies, and in the following lines
gives a beautifully poetical summary of this elevated and philosophic
discussion:--

    But whether thus these things, or whether not,
    Whether the Sun, predominant in Heaven,
    Rise on the Earth, or Earth rise on the Sun;
    He from the east his flaming round begin,
    Or she from west her silent course advance
    With inoffensive pace that spinning sleeps
    On her soft axle, whilst she paces even,
    And bears thee soft with the smooth air along--
    Solicit not thy thoughts with matters hid.--viii. 159-67.

In this scientific discourse between Adam and Raphael, in which they
discuss the structural arrangement of the heavens and the motions of
celestial bodies, we are afforded an opportunity of learning what exact
and comprehensive knowledge Milton possessed of both the Ptolemaic and
Copernican theories. The concise and accurate manner in which he
describes the doctrines belonging to each system indicates that he must
have devoted considerable time and attention to making himself master of
the details associated with both theories, which in his time were the
cause of much controversy and discussion among philosophers and men of
science.

The Ptolemaic system, with its crystalline spheres revolving round the
Earth, the addition to those of cycles and epicycles, and the heaping of
them upon each other, in order to account for phenomena associated with
the motions of celestial bodies, are concisely and accurately described.

The unreasonableness of this theory, when compared with the Copernican,
is clearly delineated by Milton where Adam is made to express his views
with regard to motion in the heavens. His argument, declared in logical
and persuasive language, demonstrates how contrary to reason it would be
to imagine that the entire heavens should revolve round the Earth to
bring about a result which could be more easily attained by imparting
motion to the Earth herself. The inconceivable velocity with which it
would be necessary for the celestial orbs to travel in order to
accomplish their daily revolution is described by him as opposed to all
reason, and entailing upon them a journey which it would be impossible
for material bodies to perform. None the less accurate is Milton's
description of the Copernican system. He describes the Sun as occupying
that position in the system which his magnitude and supreme importance
claim as his sole right, having the planets with their satellites,

    That from his lordly eye keep distance due.--iii. 578,

circling in majestic orbits around him, acknowledging his controlling
power, and bending to his firm but gentle sway. Their positions, their
paths, and their motions, real and apparent, are described in flowing
and harmonious verse.




CHAPTER IV

MILTON AND GALILEO


After the death of his mother, which occurred in 1637, Milton expressed
a desire to visit the Continent, where there were many places of
interest which he often longed to see. Having obtained the consent of
his kind and indulgent father, he set out on his travels in April 1638,
accompanied by a single man-servant, and arrived in Paris, where he only
stayed a few days. During his residence in the French capital he was
introduced by Lord Scudamore, the English Ambassador at the Court of
Versailles, to Hugo Grotius, one of the most distinguished scholars and
philosophic thinkers of his age. From Paris Milton journeyed to Nice,
where he first beheld the beauty of Italian scenery and the classic
shores of the Mediterranean Sea. From Nice he sailed to Genoa and
Leghorn, and after a short stay at those places continued his journey to
Florence, one of the most interesting and picturesque of Italian cities.
Situated in the Valley of the Arno, and encircled by sloping hills
covered with luxuriant vegetation, the sides of which were studded with
residences half-hidden among the foliage of gardens and vineyards,
Florence, besides being famed for its natural beauty, was at that time
the centre of Italian culture and learning, and the abode of men eminent
in literature and science. Here Milton remained for a period of two
months, and enjoyed the friendship and hospitality of its most noted
citizens, many of whom delighted to honour their English visitor. He was
warmly welcomed by the members of the various literary academies, who
admired his compositions and conversation; the flattering encomiums
bestowed upon him by those learned societies having been amply repaid by
Milton in choice and elegant Latin verse.

Among those who resided in the vicinity of Florence was the illustrious
Galileo, who in his sorrow-stricken old age was held a prisoner of the
Inquisition for having upheld and taught scientific doctrines which were
declared to be heretical. After his abjuration he was committed to
prison, but on the intervention of influential friends was released
after a few days' incarceration, and permitted to return to his home at
Arcetri. He was, however, kept under strict surveillance, and forbidden
to leave his house or receive any of his intimate friends without having
first obtained the sanction of the ecclesiastical authorities. After
several years of close confinement at Arcetri, during which time he
suffered much from rheumatism and continued ill-health, aggravated by
grief and mental depression consequent upon the death of his favourite
daughter, Galileo applied for permission to go to Florence in order to
place himself under medical treatment. This request was granted by the
Pope subject to certain conditions, which would be communicated to him
when he presented himself at the office of the Inquisition at Florence.
These were more severe than he anticipated. He was forbidden to leave
his house or receive any of his friends there, and those injunctions
were so strictly adhered to that during Passion Week he had to obtain a
special order so that he might be able to attend mass. At the expiration
of a few months Galileo was ordered to return to Arcetri, which he never
left again.

An affliction, perhaps the most deplorable that can happen to any human
being, was added to the burden of Galileo's misfortunes and woes. A
disorder which had some years previously injured the sight of his right
eye returned in 1636. In the following year the left eye became
similarly affected, with the result that in a few months Galileo became
totally blind. His friends at first hoped that the disease was cataract,
and that some relief might be afforded by means of an operation; but it
was discovered to be an opacity of the cornea, which at his age was
considered unamenable to treatment. This sudden and unexpected calamity
was to Galileo a most deplorable occurrence, for it necessitated the
relinquishment of his favourite pursuit, which he followed with such
intense interest and delight. His friend Castelli writes: 'The noblest
eye is darkened which Nature ever made; an eye so privileged, and gifted
with such rare qualities that it may with truth be said to have seen
more than all of those eyes who are gone, and to have opened the eyes of
all who are to come.' Galileo endured his affliction with patient
resignation and fortitude, and in the following extract from a letter by
him he acknowledges the chastening hand of a Divine Providence: 'Alas!
your dear friend and servant Galileo has become totally blind, so that
this heaven, this earth, this universe, which with wonderful
observations I had enlarged a hundred and a thousand times beyond the
belief of bygone ages, henceforward for me is shrunk into the narrow
space which I myself fill in it. So it pleases God; it shall then please
me also.' The rigorous curtailment of his liberty which prompted Galileo
to head his letters, 'From my prison at Arcetri,' was relaxed when total
blindness had supervened upon the infirmities of age. Permission was
given him to receive his friends, and he was allowed to have free
intercourse with his neighbours.

Milton, during his stay at Florence, visited Galileo at Arcetri. We are
ignorant of the details of this eventful and interesting interview
between the aged and blind astronomer and the young English poet, who
afterwards immortalised his name in heroic verse, and who in his
declining years suffered from an affliction similar to that which befel
Galileo, and to which he alludes so pathetically in the following
lines:--

                          Thee I revisit safe,
    And feel thy sovran vital lamp; but thou
    Revisitest not these eyes, that roll in vain
    To find thy piercing ray, and find no dawn;
    So thick a drop serene hath quenched their orbs,
    Or dim suffusion veiled.--iii. 21-26.

We can imagine that Galileo's astronomical views, which at that time
were the subject of much discussion among scientific men and professors
of religion, and on account of which he suffered persecution, were
eagerly discussed. It is also probable that the information communicated
by Galileo, or by some of his followers, may have persuaded Milton to
entertain a more favourable opinion of the Copernican theory. The
interesting discoveries made by Galileo with his telescope without doubt
formed a pleasant subject of conversation, and Milton enjoyed the
privilege of listening to a detailed description of these from the lips
of the aged astronomer. The telescope, its principle, its mechanism, and
the method of observing, were most probably explained to him; and we can
believe that an opportunity was afforded him of examining those in
Galileo's observatory, and of perhaps testing their magnifying power
upon some celestial object favourably situated for observation. Though
Milton has not favoured us with any details of his visit to Galileo, yet
it was one which made a lasting impression upon his mind, and was never
afterwards forgotten by him. 'There it was,' he writes, 'I found and
visited the famous Galileo, grown old, a prisoner of the Inquisition for
thinking in astronomy otherwise than the Franciscan and Dominican
licensers thought.' In years long after, when Milton, himself feeble
and blind, sat down to compose his 'Paradise Lost,' the remembrance of
the Tuscan artist and his telescope was still fresh in his memory.

By the invention of the telescope and its application to astronomical
research, a vast amount of information and additional detail have been
learned regarding the bodies which enter into the formation of the solar
system; and by its aid many new ones were also discovered. On sweeping
the heavens with the instrument, the illimitable extent of the sidereal
universe became apparent, and numberless objects of interest were
brought within the range of vision the existence of which had not been
previously imagined.

The Galilean telescope was invented in 1609. But the magnifying power of
certain lenses, and their combination in producing singular visual
effects, are alluded to in the writings of several early authors. The
value of single lenses as an aid to sight had been long known, and
spectacles were in common use in the fourteenth century. Several
mathematicians have described the wonderful optical results obtained
from glasses concave and convex, of parabolic and circular forms, and
from 'perspective glasses,' in which were embodied the principle of the
telescope. It is asserted that our countryman, Roger Bacon (1214), had
some notion of the properties of the telescope; but among those familiar
with the combination of lenses the two men who made the nearest approach
to the invention of the instrument were Baptista Porta and Gerolamo
Fracastro. The latter, who died in 1553, writes as follows: 'For which
reason those things which are seen at the bottom of water appear greater
than those which are at the top; and if anyone look through two
eye-glasses, one placed upon the other, he will see everything much
larger and nearer.' It is doubtful if Fracastro had any notion of
constructing a mechanism which might answer the purpose of a telescopic
tube. Baptista Porta (1611) is more explicit in what he describes. He
writes: 'Concave lenses show distant objects most clearly, convex those
which are nearer; whence they may be used to assist the sight. With a
concave glass distant objects will be seen, small, but distinct; with a
convex one, those near at hand, larger, but confused; if you know
_rightly_ how to combine one of each sort, you will see both far and
near objects larger and clearer.' He then goes on to say: 'I shall now
endeavour to show in what manner we may continue to recognise our
friends at the distance of several miles, and how those of weak sight
may read the most minute letters from a distance. It is an invention of
great utility, and grounded on optical principles; nor is at all
difficult of execution; but it must be so divulged as not to be
understood by the vulgar, and yet be clear to the sharp-sighted.' After
this, he proceeds to describe a mechanism the details of which are
confusing and unintelligible, nor did it appear to bear any resemblance
to a telescopic tube.

In a work published by Thomas Digges in 1591, he makes the following
allusion to his father's experiments with the lenses: 'My father, by his
continuall painfull practices, assisted with demonstrations
mathematicall, was able, and sundry times hath by proportionall glasses,
duely situate in convenient angles, not only discouered things farre
off, read letters, numbered peeces of money with the verye coyne and
superscription thereof cast by some of his freends of purpose, upon
downes in open fields; but also seuen miles off, declared what hath beene
doone at that instant in priuate places.' It must be admitted that if
Leonard Digges had not constructed a telescope, he knew how to combine
lenses by the aid of which a visual effect was created similar to that
produced by the use of the instrument.

The inventor of the telescope was a Dutchman named Hans Lippershey, who
carried on the business of a spectacle-maker in the town of Middelburg.
His discovery was purely accidental. It is said that the
instrument--which was directed towards a weather-cock on a church spire,
of which it gave a large and inverted image--was for some time exhibited
in his shop as a curiosity before its importance was recognised. The
Marquis Spinola, happening to see this philosophical toy, purchased it,
and presented it to Prince Maurice of Nassau, who imagined it might be
of service for the purpose of military reconnoitring. The value of the
invention was, however, soon realised, and in the following year
telescopes were sold in Paris. In 1609, Galileo, when on a visit to a
friend at Venice, received intelligence of the invention of an
instrument by a Dutch optician which possessed the power of causing
distant objects to appear much nearer than when observed by ordinary
vision. The accuracy of this information was confirmed by letters which
he received from Paris; and this general report, Galileo asserted, was
all he knew of the subject. Fuccarius, in a disparaging letter, says
that one of the Dutch telescopes had been brought to Venice, and that he
himself had seen it. This statement is not incompatible with Galileo's
affirmation that he had not seen the original instrument, and knew no
more about it than what had been communicated to him in the letters from
the French capital. It was insinuated by Fuccarius that Galileo had seen
the telescope at Venice, but, as he denied this, we should not hesitate
to believe in his veracity.

Immediately after his return to Padua, Galileo began to think how he
might be able to contrive an instrument with properties similar to the
one of which he had been informed; and in the following words describes
the process of reasoning by which he arrived at a successful result: 'I
argued in the following manner. The contrivance consists either of one
glass or of more--one is not sufficient, since it must be either convex,
concave, or plane. The last does not produce any sensible alteration in
objects; the concave diminishes them. It is true that the convex
magnifies, but it renders them confused and indistinct; consequently,
one glass is insufficient to produce the desired effect. Proceeding to
consider two glasses, and bearing in mind that the plane causes no
change, I determined that the instrument could not consist of the
combination of a plane glass with either of the other two. I therefore
applied myself to make experiments on combinations of the two other
kinds, and thus obtained that of which I was in search.' Galileo's
telescope consisted of two lenses--one plano-convex, the other
plano-concave, the latter being held next the eye. These he fixed in a
piece of organ pipe, which served the purpose of a tube, the glasses
being distant from each other by the difference of their focal lengths.
An exactly similar principle is adopted in the construction of an
opera-glass, which can be accurately described as a double Galilean
telescope. Galileo must be regarded as the inventor of this kind of
telescope, which in one respect differed very materially from the one
constructed by the Dutch optician. If what has been said with regard to
the _inverted_ weather-cock be true, then Lippershey's telescope was
made with two convex lenses, distant from each other by the sum of their
focal lengths, and all objects observed with it were seen inverted.
Refracting astronomical telescopes are now constructed on this
principle, it having been discovered that for observational purposes
they possess several advantages over the Galilean instrument. When
Galileo had completed his first telescope he returned with it to
Venice, where he exhibited it to his friends. The sensation created by
this small instrument, which magnified only three times, was most
extraordinary, and almost amounted to a frenzy. Crowds of the principal
citizens of Venice flocked to Galileo's house in order that they might
see the magical tube about which such wonderful reports were circulated;
and for upwards of a month he was daily occupied in describing his
invention to attentive audiences. At the expiration of this time the
Doge of Venice, Leonardo Deodati, hinted that the Senate would not be
averse to receive the telescope as a gift. Galileo readily acquiesced
with this desire, and, as an acknowledgment of his merits, a decree was
issued confirming his appointment as professor at Padua for life, and
increasing his salary from 500 to 1,000 florins. The public excitement
created by the telescope showed no signs of abatement. Sirturi mentions
that, having succeeded in constructing an instrument, he ascended the
tower of St. Mark's at Venice, hoping to be able to use it there without
interruption. He was, however, detected by a few individuals, and soon
surrounded by a crowd, which took possession of his telescope, and
detained him for several hours until their curiosity was satisfied.
Eager inquiries having been made as to where he lodged, Sirturi, fearing
a repetition of his experience in the church tower, decided to quit
Venice early next morning, and betake himself to a quieter and less
frequented neighbourhood.

The instrument was at first called Galileo's tube; the double eye-glass;
the perspective; the trunk; the cylinder. The appellation _telescope_
was given it by Demisiano.

Galileo next directed his attention to the construction of telescopes,
and applied his mechanical skill in making instruments of a larger size,
one of which magnified _eight_ times. 'And at length,' he writes,
'sparing neither labour nor expense, he completed an instrument that was
capable of magnifying more than _thirty_ times.'

Galileo now commenced an exploration of the celestial regions with his
telescope, and on carefully examining some of the heavenly bodies, made
many wonderful discoveries which added greatly to the fame and lustre of
his name.

The first celestial object to which Galileo directed his telescope was
the Moon. He was deeply interested to find how much her surface
resembled that of the Earth, and was able to perceive lofty mountain
ranges, the illumined peaks of which reflected the sunlight, whilst
their bases and sides were still enveloped in dark shadow; great plains
which he imagined were seas, valleys, elevated ridges, depressions, and
inequalities similar to what are found on our globe. Galileo believed
the Moon to be a habitable world, and concluded that the dark and
luminous portions of her surface were land and water, which reflected
with unequal intensity the light of the Sun. The followers of Aristotle
received the announcement of these discoveries with much displeasure.
They maintained that the Moon was perfectly spherical and smooth--a vast
mirror, the dark portions of which were the reflection of our
terrestrial mountains and forests--and accused Galileo 'of taking a
delight in distorting and ruining the fairest works of Nature.' He
appealed to the unequal condition of the surface of our globe, but this
was of no avail in altering their preconceived notions of the lunar
surface.

Perhaps the most important discovery made by Galileo with the telescope
was that of the four moons of Jupiter. On the night of January 7, 1610,
when engaged in observing the planet, his attention was attracted by
three small stars which appeared brighter than those in their immediate
neighbourhood. They were all in a straight line and parallel with the
ecliptic; two of them were situated to the east, and one to the west of
Jupiter. On the following night he was surprised to find all three to
the west of the planet, and nearer to each other. This caused him
considerable perplexity, and he was at a loss to understand how Jupiter
could be east of the three stars, when on the preceding night he was
observed to the west of two of them. Galileo was unable to reconcile the
altered positions of those bodies with the apparent motion of Jupiter
among the fixed stars as indicated by the astronomical tables. The next
opportunity he had of observing them was on the 10th, when two stars
only were visible, and they were to the east of the planet. As it was
impossible for Jupiter to move from west to east on January 8 and from
east to west on the 10th, he concluded that it was the motion of the
stars and not that of Jupiter which accounted for the observed
phenomena. Galileo watched the stars attentively on successive evenings
and discovered a fourth, and on observing how they changed their
positions relatively to each other he soon arrived at the conclusion
that the stars were four moons which revolved round Jupiter after the
manner in which the Moon revolves round the Earth. Having assured
himself that the four new stars were four moons that with periodical
regularity circled round the great planet, Galileo named them the
Medicean Stars in honour of his patron, Cosmo de' Medici, Grand Duke of
Tuscany. He also published an essay entitled 'Nuncius Sidereus,' or the
'Sidereal Messenger,' which contained an account of this important
discovery.

The announcement of Galileo's discovery of the four satellites of
Jupiter created a profound sensation, and its significance became at
once apparent. Aristotelians and Ptolemaists received the information
with much disfavour and incredulity, and many persons positively refused
to believe Galileo, whom they accused of inventing fables. On the other
hand, the upholders of the Copernican theory hailed it with
satisfaction, as it declared that Jupiter with his four moons
constituted a system of greater magnitude and importance than that of
our globe with her single satellite, and that consequently the Earth
could not be regarded as the centre of the universe.

When Kepler heard of this remarkable discovery, he wrote to Galileo and
expressed himself in the following characteristic manner: 'I was sitting
idle at home thinking of you, most excellent Galileo, and your letters,
when the news was brought me of the discovery of four planets by the
help of the double eye-glass. Wachenfels stopped his carriage at my door
to tell me, when such a fit of wonder seized me at a report which seemed
so very absurd, and I was thrown into such agitation at seeing an old
dispute between us decided in this way, that between his joy, my
colouring, and the laughter of both, confounded as we were by such a
novelty, we were hardly capable, he of speaking, or I of listening.... I
am so far from disbelieving in the existence of the four circumjovial
planets, that I long for a telescope to anticipate you, if possible, in
discovering two round Mars (as the proportion seems to me to require),
six or eight round Saturn, and perhaps one each round Mercury and
Venus.' The intelligence of Galileo's discoveries was received by his
opponents in a spirit entirely different from that manifested by Kepler.
The principal professor of philosophy at Padua, when requested to look
at the Moon and planets through Galileo's glass, persistently declined,
and did his utmost to persuade the Grand Duke that the four satellites
of Jupiter could not possibly exist. Francesco Sizzi, a Florentine
astronomer, argued that, as there are seven apertures in the head,
seven known metals, and seven days in the week, so there could only be
seven planets. To these absurd remarks Galileo replied by saying that,
'whatever their force might be as a reason for believing beforehand that
no more than seven planets would be discovered, they hardly seemed of
sufficient weight to destroy the new ones when actually seen.' Another
individual, named Christmann, writes: 'We are not to think that Jupiter
has four satellites given him by Nature in order, by revolving round
him, to immortalize the name of the Medici, who first had notice of the
observation. These are the dreams of idle men, who love ludicrous ideas
better than our laborious and industrious correction of the heavens.
Nature abhors so horrible a chaos, and to the truly wise such vanity is
detestable.' Martin Horky, a _protégé_ of Kepler's, issued a pamphlet in
which he made a violent attack on Galileo. He says: 'I will never
concede his four new planets to that Italian from Padua though I die for
it.' He then asks the following questions, and replies to them himself:
(1) Whether they exist? (2) What they are? (3) What they are like? (4)
Why they are? 'The first question is soon disposed of by Horky's
declaring positively that he has examined the heavens with Galileo's own
glass, and that no such thing as a satellite about Jupiter exists. To
the second, he declared solemnly that he does not more surely know that
he has a soul in his body than that reflected rays are the sole cause of
Galileo's erroneous observations. In regard to the third question, he
says that these planets are like the smallest fly compared to an
elephant; and, finally, concludes on the fourth, that the only use of
them is to gratify Galileo's "thirst of gold," and to afford himself a
subject of discussion.'[7] Galileo did not condescend to take any notice
of this scurrilous production; but Horky, who imagined that he had done
something clever, sent a copy of his pamphlet to Kepler. In a few days
after he called to see him, and was received with such a storm of
indignation that he begged for mercy and implored his forgiveness.
Kepler forgave him, but insisted on his making amends. He writes: 'I
have taken him again into favour upon this preliminary condition, to
which he has agreed--that I am to show him Jupiter's satellites, _and he
is to see them_, and own that they are there.'

The evidence in support of the existence of Jupiter's satellites became
so conclusive that the opponents of Galileo were compelled to renounce
their disbelief in those bodies, whether real or pretended. The Grand
Duke, preferring to trust to his eyes rather than believe in the
arguments of the professor at Padua, observed the satellites on several
occasions, along with Galileo, at Pisa, and on his departure bestowed
upon him a gift of one thousand florins. Several of Galileo's enemies,
as a result of their observations, now arrived at the conclusion that
his discovery was incomplete, and that Jupiter had more than four
satellites in attendance upon him. Scheiner counted five, Rheita nine,
and other observers increased the number to twelve. But it was found to
be quite as hazardous to exceed the number stated by Galileo as it was
to deny the existence of any; for, when Jupiter had traversed a short
distance of his path among the fixed stars, the only bodies that
accompanied him were his four original attendants, which continued to
revolve round him with unerring regularity in every part of his orbit.

Galileo did not afford his opponents much time to oppose or controvert
with argument the discoveries made by him with the telescope before his
announcement of a new one attracted public attention from those already
known. He, however, exercised greater caution in disclosing the results
of his observations, as other persons laid claim to having made similar
discoveries prior to the time at which his were announced. He therefore
adopted a method in common use among astronomers in those days, by which
the letters in a sentence announcing a discovery were transposed so as
to form an anagram.

Galileo announced his next discovery in this manner, and which read as
follows:--

    Smaismrmilme poeta leumi bvne nugttaviras.

This, when deciphered, formed the sentence:--

    Altissimum planetam tergeminum observavi.

    I have observed that the remotest planet is triple.

Galileo perceived that Saturn presented a triform appearance, and that,
instead of one body, there were three, all in a straight line, and
apparently in contact with each other, the middle one being larger than
the two lateral ones. In a letter to Kepler he remarked: 'Now I have
discovered a Court for Jupiter, and two servants for this old man, who
aid his steps and never quit his side.' Kepler, who excelled as an
imaginative writer, replied: 'I will not make an old man of Saturn, nor
slaves of his attendant globes; but rather let this tricorporate form be
Geryon--so shall Galileo be Hercules, and the telescope his club, armed
with which he has conquered that distant planet, and dragged him from
the remotest depths of Nature, and exposed him to the view of all.'
Continuing his observations, Galileo perceived that the two lateral
objects gradually decreased in size, and at the expiration of two years
entirely disappeared, leaving the central globe visible only. He was
unable to assign any reason for this peculiar occurrence, which caused
him much perplexity, and he expresses himself thus: 'What is to be said
concerning so strange a metamorphosis? Are the two lesser stars consumed
after the manner of the solar spots? Have they vanished and suddenly
fled? Has Saturn, perhaps, devoured his own children? Or were the
appearances, indeed, illusion or fraud, with which the glasses have so
long deceived me, as well as many others to whom I have shown them? Now,
perhaps, is the time to revive the well-nigh withered hopes of those
who, guided by more profound contemplations, have discovered the fallacy
of the new observations, and demonstrated the utter impossibility of
their existence. I do not know what to say in a case so surprising, so
unlooked-for, and so novel. The shortness of the time, the unexpected
nature of the event, the weakness of my understanding, and the fear of
being mistaken, have greatly confounded me.' After a certain interval
those bodies reappeared; but Galileo's glass was not sufficiently
powerful to enable him to ascertain their nature nor solve the mystery,
which for upwards of half a century perplexed the ablest astronomers.

The elucidation of this inexplicable phenomenon was reserved for
Christian Huygens, who, with an improved telescope of his own
construction, was able to declare that Saturn's appendages were portions
of a ring which surrounds the planet, and is everywhere distinct from
its surface.

Galileo next directed his attention to the planet Venus, and as a result
of his observations was led to communicate to the public another
anagram:--

    Haec immatura a me jam frustra leguntur oy.

This, when rendered correctly, reads:--

    Cynthiae figuras aemulatur mater amorum.

    Venus rivals the appearances of the Moon.

The phases of Venus were one of the most interesting of Galileo's
discoveries with the telescope. When observed near inferior conjunction
the planet presents the appearance of a slender crescent, resembling
the Moon when a few days old. Travelling from this point to superior
conjunction, the illumined portion of her disc gradually increases,
until it becomes circular, like the full Moon. This changing appearance
of Venus afforded Galileo irresistible proof that the planet is an
opaque body, which derives its light from the Sun, and that it circles
round the orb--convincing evidence of the accuracy and truthfulness of
the Copernican theory.

It was in this manner that Galileo announced his discovery of the phases
of Venus, the peerless planet of our morning and evening skies, whose
slender crescent forms such a beautiful object in the telescope, and
who, as she traverses her orbit, exhibits all the varied changes of form
presented by the Moon in her monthly journey round the Earth. These
varying aspects of Venus were not unknown to Milton; and, indeed, he may
have been informed of them by Galileo in his conversation with him at
Arcetri; nor has he failed to introduce an allusion to this beautiful
phenomenon in his poem. In his description of the Creation, after the
Sun was formed, he adds:--

    Hither, as to their fountain, other stars
    Repairing, in their golden urns draw light,
    And hence the morning planet gilds her horns.--vii. 364-66.

Galileo also discovered that the planet Mars does not always present the
appearance of a circular disc. When near opposition the full disc of the
planet is visible, but at all other times it is gibbous, and approaches
nearest to that of a half-moon when at the quadratures.

In the year 1610, on directing his telescope to the Sun, Galileo
detected dark spots on the solar disc. Similar spots, sufficiently large
to be distinguished by the naked eye, had been observed from time to
time for centuries prior to the invention of the telescope, but nothing
was known of their nature. In 1609 Kepler observed a spot on the Sun,
which he thought was the planet Mercury in conjunction with the orb; the
short time during which it was visible, in consequence of clouds having
obscured the face of the luminary, prevented him from being able to
determine the accuracy of his surmise, but since then it has been
ascertained that no transit of Mercury took place at that time, and
Kepler afterwards acknowledged that he had arrived at an erroneous
conclusion. Galileo was much puzzled in trying to find out the true
nature of the spots. At first he was led to imagine that planets like
Mercury and Venus revolved round the Sun at a short distance from the
orb, and that their dark bodies, travelling across the solar disc, gave
rise to the phenomenon of the spots. After further observation, he
ascertained that the spots were in actual contact with the Sun; that
they were irregular in shape and size, and continued to appear and
disappear. Sometimes a large spot would break up into several smaller
ones, and at other times three or four small spots would unite to form a
large one. They all had a common motion, and appeared to rotate with
the Sun, from which Galileo concluded that the orb rotated on his axis
in about twenty-eight days. Galileo believed that the spots were clouds
floating in the solar atmosphere, and that they intercepted a portion of
the light of the Sun.

The Milky Way, that wondrous zone of light which encircles the heavens,
remained for many ages a source of perplexity to ancient astronomers and
philosophers, who, in their endeavours to ascertain its nature, had
arrived at various absurd and erroneous conclusions. On directing his
telescope to this luminous tract, Galileo discovered, to his
inexpressible admiration, that it consists of a vast multitude of stars,
too minute to be visible to the naked eye. He also discerned that its
milky luminosity is created by the blended light of myriads of stars, so
remote as to be incapable of definition by his telescope. In his
'Nuncius Sidereus' he gives an account of his observations of the Galaxy
and expresses his satisfaction that he has been enabled to terminate an
ancient controversy by demonstrating to the senses the stellar structure
of the Milky Way. When engaged in exploring the celestial regions with
his telescope, Galileo observed a marked difference in the appearance of
the fixed stars, as compared with that of the planets. Each of the
latter showed a rounded disc resembling that of a small moon, but the
stars exhibited no disc, and shone as vivid sparkling points of light;
all of them, whether of large or small magnitude, presenting the same
appearance in the telescope. This led him to conclude that the fixed
stars were not illumined by the Sun, because their brilliancy in all
their changes of position remained unaltered. But, in the case of the
planets, he found that their lustre varied according to their distance
from the Sun; consequently, he believed they were opaque bodies which
reflected the solar rays. On directing his telescope to the Pleiades,
which, to the naked eye, appear as a group of seven stars, he succeeded
in counting forty lucid points. The nebula Praesepe in Cancer, he was
also able to resolve into a cluster of stars. Galileo made many other
observations of the heavenly bodies with his telescope, all of which he
describes as having afforded him 'incredible delight.'

Shortly before the failure of his eyesight, Galileo discovered the
Moon's diurnal libration, a variation in the visible edges of the Moon
caused by its oscillatory motion, and the diurnal rotation of the Earth
on her axis.

Though Milton has not favoured us with any interesting details of his
interview with Galileo, nor expressed his opinions with regard to the
controversies which at that time agitated both the religious and
scientific worlds of thought, and which eventually culminated in a storm
of rancour and hatred that burst over the devoted head of the aged
astronomer, and brought him to his knees, yet he informs us that he
'found and visited' Galileo, whom he describes as 'grown old,' and
cynically remarks that he 'was held a prisoner of the Inquisition for
thinking in astronomy otherwise than the Franciscan and Dominican
licensers thought.' Milton does not allude to his blindness, and yet it
would be natural to imagine that, had his host suffered from this
affliction at the time of his visit, he would have referred to it. We
learn that Milton arrived in Italy in the spring of 1638. In 1637, the
affection which, in the preceding year, deprived Galileo of the use of
his right eye, attacked the left also, which began to grow dim, and in
the course of a few months became sightless; so that, although Milton
has not alluded to this calamity, Galileo had become totally blind at
the time of his visit.

How much Milton was impressed with the fame of Galileo and his telescope
becomes apparent on referring to his 'Paradise Lost.' In it he alludes
to the instrument upon three different occasions, twice when in the
hands of Galileo; and the remembrance of the same artist was doubtless
in his mind when he mentions the 'glazed optic tube' in another part of
his poem. The interval that elapsed from the date of Milton's visit to
Galileo in 1638, to the publication of 'Paradise Lost' in 1667, included
a period of about thirty years, yet this length of time did not erase
from Milton's memory his recollection of Galileo and of his pleasant
sojourn at Florence.

The first allusion in the poem to the Italian astronomer is in the lines
in which Milton describes the shield carried by Satan:--

                      The broad circumference
    Hung on his shoulders like the Moon, whose orb
    Through optic glass the Tuscan artist views
    At evening, from the top of Fesolé,
    Or in Valdarno, to descry new lands,
    Rivers, or mountains, in her spotty globe.--i. 286-91.

Galileo is described as having observed the Moon from the heights of
Fesolé, which formed part of the suburbs of Florence, or from Valdarno,
the valley of the Arno, in which the city is situated. The belief that
Galileo had discovered continents and seas on the Moon justified Milton
in imagining the existence of rivers and mountains on the lunar surface.
The expression 'spotty globe' is more descriptive of the appearance of
our satellite when observed with the telescope, than when seen with the
naked eye. Galileo's attention was attracted by the freckled aspect of
the Moon--a visual effect created by the number of extinct volcanoes
scattered over the surface of the orb.

In his next allusion to the telescope Milton associates Galileo's name
with the instrument:--

                      As when by night the glass
    Of Galileo, less assured, observes
    Imagined lands and regions in the Moon.--v. 261-63.

In these lines Milton describes with accuracy the extent of Galileo's
knowledge of our satellite. The conclusions which the Italian astronomer
arrived at with regard to its habitability were not supported by
telescopic evidence sufficient to justify such a belief. Galileo writes:
'Had its surface been absolutely smooth it would have been but a vast,
unblessed desert, void of animals, of plants, of cities and men; the
abode of silence and inaction--senseless, lifeless, soulless, and
stripped of all those ornaments which now render it so variable and so
beautiful:'--

    There lands the Fiend, a spot like which perhaps
    Astronomer in the Sun's lucent orb
    Through his glazed optic tube yet never saw.--iii. 588-90.

Milton may have remembered that Galileo was the first astronomer who
directed a telescope to the Sun; and that he discovered the dark spots
frequently seen on the solar disc.

Anyone who has read a history of the life of Galileo, and contemplated
the career of this remarkable man, his ardent struggles in the cause of
freedom and philosophic truth, his victories and reverses, his brilliant
astronomical discoveries, and his investigation of the laws of motion,
and other natural phenomena, will arrive at the conclusion that he
merited the distinction conferred upon him by our great English poet,
when he included him among the renowned few whose names are found in the
pages of 'Paradise Lost.'




CHAPTER V

THE SEASONS


The great path of the Sun among the constellations as seen from the
Earth is called the Ecliptic. It is divided into 360°, and again into
twelve equal parts of 30°, called Signs. As one half of the ecliptic is
north, and the other half south, of the equator, the line of
intersection of their planes is at two points which are known as the
equinoctial points, because, when the Sun on his upward and downward
journey arrives at either of them the days and nights are of equal
length all over the world. The equinoctial points are not stationary,
but have a westerly motion of 50´´ annually along the ecliptic; at this
rate they will require a period of 25,868 years to complete an entire
circuit of the heavens.

Milton alludes to the ecliptic when he mentions the arrival of Satan
upon the Earth:--

    Down from the ecliptic, sped with hoped success,
    Throws his steep flight in many an airy wheel,
    Nor staid till on Niphates top he lights.--iii. 740-42.

Extending for 9° on each side of the ecliptic is a zone or belt called
the Zodiac, the mesial line of which is occupied by the Sun, and within
this space the principal planets perform their annual revolutions. It
was for long believed that the paths of all the planets lay within the
zodiac, but on the discovery of the minor planets, Ceres, Pallas, and
Juno, it was ascertained that they travelled beyond this zone. The stars
situated within the zodiac are divided into twelve groups or
constellations, which correspond with the twelve signs, and each is
named after an animal or some figure which it is supposed to resemble.
The zodiac is of great antiquity; the ancient Egyptians and Hindoos made
use of it, and there are allusions to it in the earliest astronomical
records. The twelve constellations of the zodiac bear the following
names:--

Aries the Ram
Taurus the Bull
Gemini the Twins
Cancer the Crab
Leo the Lion
Virgo the Virgin
Libra the Balance
Scorpio the Scorpion
Sagittarius the Archer
Capricornus the Goat
Aquarius the Water-bearer
Pisces the Fishes

In close association with the Sun's annual journey are the seasons, upon
the regular sequence of which mankind depend for the various products of
the soil essential for the maintenance and enjoyment of life. The
revolution of the Earth in her orbit, and the inclination of her axis to
her annual path, causing the plane of the equator to be inclined 23-1/2°
to that of the ecliptic, are the reasons which account for the
succession of the seasons--Spring, Summer, Autumn, and Winter. Owing to
the position of the Earth's axis with regard to her orbit, the Sun
appears to travel 23-1/2° north and 23-1/2° south of the equator. When,
on June 21, the orb attains his highest northern altitude, we have the
summer solstice and the longest days; when, by retracing his steps, he
declines 23-1/2° below the equator, at which point he arrives on
December 21, we have the winter solstice and the shortest days.
Intermediate between those two seasons are spring and autumn. When the
Sun, on his journey northward, reaches the equator, we have the vernal
equinox, and at this period of the year the days and nights are of equal
length all over the globe. In a similar manner, when, on his return
journey, the Sun is again on the equator, the autumnal equinox occurs.
In summer the North Pole is inclined towards the Sun, consequently his
rays fall more direct and impart much more heat to the northern
hemisphere than in winter, when the Pole is turned away from the Sun.
This difference in the incidence of the solar rays upon the surface of
the globe, along with the increased length of the day, mainly accounts
for the high temperature of summer as compared with that of winter.

Astronomically, the seasons commence at the periods of the equinoxes and
solstices. Spring begins on March 21, the time of the vernal equinox;
summer on June 21, at the summer solstice; autumn on September 22, at
the autumnal equinox; and winter on December 21, at the winter solstice.
This conventional division of the year is not equally applicable to all
parts of the globe. In the arctic and antarctic regions spring and
autumn are very brief, the summer is short and the winter of long
duration. In the tropics, owing to the comparatively slight difference
in the obliquity of the Sun's rays, one season is, as regards
temperature, not much different from the other; but in the temperate
regions of the Earth the vicissitudes of the seasons are more
perceptible and can be best distinguished by the growth of vegetation,
and the changes observable in the foliage of shrubs and trees. In spring
there is the budding, in summer the blossom, in autumn the
fruit-bearing, and in winter the leafless condition of deciduous trees,
and the repose of vegetable life.

The legendary belief that before the Fall there reigned on the Earth a
perpetual spring, is introduced by Milton in his poem when he describes
the pleasant surroundings associated with the happy conditions of life
that existed in Paradise:--

                                Thus was this place,
    A happy rural seat of various view:
    Groves whose rich trees wept odorous gums and balm;
    Others whose fruit, burnished with golden rind,
    Hung amiable--Hesperian fables true,
    If true here only--and of delicious taste.
    Betwixt them lawns, or level downs, and flocks
    Grazing the tender herb, were interposed,
    Or palmy hillock; or the flowery lap
    Of some irriguous valley spread her store,
    Flowers of all hue, and without thorn the rose.
    Another side, umbrageous grots and caves
    Of cool recess, o'er which the mantling vine
    Lays forth her purple grape, and gently creeps
    Luxuriant; meanwhile murmuring waters fall
    Down the slope hill dispersed, or in a lake
    That to the fringèd bank with myrtle crowned
    Her crystal mirror holds, unite their streams.
    The birds their quire apply; airs, vernal airs,
    Breathing the smell of field and grove, attune
    The trembling leaves, while universal Pan,
    Knit with the Graces and the Hours in dance,
    Led on the eternal Spring.--iv. 246-68.

In sad contrast with this charming sylvan scene, we turn to the unhappy
consequences which ensued as a result of the first act of transgression.
Milton describes a change of climate characterised by extremes of heat
and cold which succeeded the perpetual spring. The Sun was made to shine
so that the Earth should be exposed to torrid heat and icy cold
unpleasant to endure. The pale Moon and the planets were given power to
combine with noxious effect, and the fixed stars to shed their malignant
influences:--

                                            The Sun
    Had first his precept so to move, so shine,
    As might affect the Earth with cold and heat
    Scarce tolerable, and from the north to call
    Decrepit winter, from the south to bring
    Solstitial summer's heat. To the blanc Moon
    Her office they prescribed; to the other five
    Their planetary motions and aspects,
    In sextile, square, and trine, and opposite,
    Of noxious efficacy, and when to join
    In synod unbenign; and taught the fixed
    Their influence malignant when to shower--
    Which of them rising with the Sun or falling,
    Should prove tempestuous. To the winds they set
    Their corners, when with bluster to confound
    Sea, air, and shore; the thunder when to roll
    With terror through the dark aerial hall.--x. 651-67.

We are here afforded an opportunity of learning that Milton possessed
some knowledge of astrology, to which he makes allusion in other parts
of his poem besides. In his time, astrology was believed in by many
persons, and there were few learned men but who knew something of that
occult science. Milton may be included among those who devoted some
attention to astrology. Of this there is ample evidence, by the manner
in which he expresses himself in words and phrases in common use among
astrologers.

The professors of this art recognised five planetary aspects, viz.,
opposition, conjunction, sextile, square, and trine, each possessing its
peculiar kind of influence on events. The Moon, the planets, and the
constellations in their conjunctions and configurations, were believed
to reveal to those who could understand the significance of their
aspects, the destiny of individuals and the occurrence of future events.
The inauspicious influences of the heavenly bodies are described by
Milton as contributing to the general disarrangement of the happy
condition of things that existed before the Fall.

After having described the adverse physical changes which occurred in
Nature as a consequence of the Fall, Milton makes use of his
astronomical knowledge in explaining how they were brought about, and
suggests two hypotheses: (1) a change of position of the Earth's axis;
(2) an alteration of the Sun's path from the equinoctial road:--

    Some say he bid his Angels turn askance
    The poles of Earth twice ten degrees and more
    From the Sun's axle; they with labour pushed
    Oblique the centric globe: some say the Sun
    Was bid turn reins from the equinoctial road
    Like distant breadth--to Taurus with the seven
    Atlantic Sisters, and the Spartan Twins,
    Up to the Tropic Crab; thence down amain
    By Leo, and the Virgin, and the Scales,
    As deep as Capricorn; to bring in change
    Of seasons to each clime. Else had the spring
    Perpetual smiled on Earth with vernant flowers.--x. 668-79.

In support of the theory of a perpetual spring, Milton assumes that the
Earth's axis was directed at right angles to her orbit, and that the
plane of the equator coincided with that of the ecliptic. Consequently,
the Sun's path remained always on the equator, where his rays were
vertical, and north and south of this line each locality on the Earth
enjoyed one constant season, the character of which depended upon its
geographical position. In what are now the temperate regions of the
globe there was one continuous season, similar in climate and length of
day to what is experienced at the vernal equinox, when the Sun is for a
few days on the equator. There was then no winter, no summer, nor
autumn; and, consequently, the growth of vegetation must have taken
place under conditions of climate entirely different to what exist on
the Earth at the present time.

The change of position of the Earth's axis, 'twice ten degrees and more
from the Sun's axle,' is described by Milton as having been
accomplished by the might of angels, who 'with labour pushed oblique the
centric globe.'

(2) According to the Ptolemaic belief, the Sun revolved round the Earth,
but his course was altered from the equinoctial road to the path that he
now pursues, which is the ecliptic. Instead of remaining on the equator,
he travels an equal distance from this line upwards and downwards in
each hemisphere.

The path of the Sun in the heavens is described by Milton with marked
precision, and he mentions in regular order the names of the zodiacal
constellations through which the orb travels. Passing through Taurus
with the seven Atlantic Sisters (the Pleiades) and the Spartan Twins
(Gemini), he enters the Tropic Crab (Cancer), in which constellation he
attains his highest northern altitude; thence downwards he travels
through Leo, Virgo, and the Scales (Libra), as deep as Capricornus,
reaching his lowest point of declination at the winter solstice; and
were it not for this alteration of the Sun's path, the poet informs us
that perpetual spring would have reigned upon the Earth.

Milton was evidently well acquainted with the astronomical reasons (the
revolution of the Earth in her orbit and the obliquity of the ecliptic)
by which the occurrence and regular sequence of the seasons can be
explained.

The path of the Sun in the heavens; his upward and downward course from
the equator; the names of the constellations through which the orb
travels, and the periods of the year at which he enters them, were also
familiar to him.

The grateful change of the seasons, and the varied aspects of nature
peculiar to each, which give a charm and freshness to the rolling year,
must have been to Milton a source of pleasure and delight, and have
stimulated his poetic fancy.

His observation of natural phenomena, and his keen perception of the
pleasing changes which accompany them, are described in the following
lines:--

    As, when from mountain-tops the dusky clouds
    Ascending, while the north wind sleeps, o'erspread
    Heaven's cheerful face, the louring element
    Scowls o'er the darkened landskip snow or shower,
    If chance the radiant Sun, with farewell sweet,
    Extend his evening beam, the fields revive,
    The birds their notes renew, and bleating herds
    Attest their joy, that hill and valley rings.--ii. 488-95.

The ancient poets Virgil and Ovid describe the Earth as having been
created in the spring; and associated with this season, which

                    to the heart inspires
    Vernal delight and joy--iv. 154-55,

were the Graces and the Hours, which danced hand in hand as they led on
the eternal Spring.

Milton alludes to the seasons on several occasions throughout his poem,
and to the natural phenomena associated with them:--

                                        As bees
    In springtime when the Sun with Taurus rides,
    Pour forth their populous youth about the hive
    In clusters; they among fresh dews and flowers
    Fly to and fro, or on the smoothèd plank
    The suburb of their straw-built citadel
    New rubbed with balm, expatiate and confer
    Their state affairs.--i. 768-75.

The Sun is in the constellation Taurus in April, when the warmth of his
rays begins to impart new life and activity to the insect world after
their long winter's sleep.

In his description of the repast partaken by the Angel Raphael with Adam
and Eve in Paradise, Milton writes:--

                              Raised of grassy turf
    Their table was, and mossy seats had round,
    And on her ample square, from side to side,
    All Autumn piled, though Spring and Autumn here
    Danced hand in hand.--v. 391-95.

In describing Beelzebub when about to address the Stygian Council, he
says:--

                                          His look
    Drew audience and attention still as night
    Or summer's noontide air, while thus he spake.--ii. 307-309.

The failing vision from which Milton suffered in his declining years was
succeeded by total blindness. This sad affliction he alludes to in the
following lines:--

                              Thus with the year
    Seasons return; but not to me returns
    Day, or the sweet approach of even or morn,
    Or sight of vernal bloom, or summer's rose.--iii. 40-43.

We are able to perceive how much Milton was impressed with the beautiful
seasons, and the varying aspects of the year which accompany them, and
how his poetic imagination luxuriated in the changing variety of nature
observable in earth and sky that from day to day afforded him exquisite
delight; and, although his poem was written when blindness had overtaken
him, yet those glad remembrances remained as fresh in his memory as when
in his youth he roamed among the flowery meadows, the vocal woodlands,
and the winding lanes of Buckinghamshire.

The idea expressed by Milton that the primitive earth enjoyed a
perpetual spring, though pleasing to the imagination, and well adapted
for poetic description, is not sustained by any astronomical testimony.
Indeed, the position of the Earth, with her axis at right angles to her
orbit, is one which may be regarded as being ill adapted for the support
and maintenance of life on her surface, just as her present position is
the best that can be imagined for fulfilling this purpose.

Astronomy teaches us to rely with certainty upon the permanence and
regular sequence of the seasons. The position of the Earth's axis as she
speeds along in her orbit through the unresisting ether remains
unchanged, and her rapid rotation has the effect of increasing its
stability. Yet, the Earth performs none of her motions with rigid
precision, and there is a very slow alteration of the position of her
axis occurring, which, if unchecked, would eventually produce a
coincidence of the equator and the ecliptic. Instead of a succession of
the seasons, there would then be perpetual spring upon the Earth, and,
although it would require a great epoch of time to bring about such a
change, there would result a condition of things entirely different to
what now exists on the globe. But, before the ecliptic can have
approached sufficiently near the equator to produce any appreciable
effect upon the climate of the Earth, its motion must cease, and after
remaining stationary for a time, it will begin to recede to its former
position. The seasons must therefore follow each other in regular
sequence, and throughout all time, reminding us of the promise of the
Creator, 'that while the Earth remaineth seed-time and harvest, and cold
and heat, and summer and winter shall not cease.'




CHAPTER VI

THE STARRY HEAVENS


The celestial vault, that, like a circling canopy of sapphire hue,
stretches overhead from horizon to horizon, resplendent by night with
myriad stars of different magnitudes and varied brilliancy, forming
clusterings and configurations of fantastic shape and beauty, arrests
the attention of the most casual observer. But to one who has studied
the heavens, and followed the efforts of human genius in unravelling the
mysteries associated with those bright orbs, the impression created on
his mind as he gazes upon them in the still hours of the night, when the
turmoil of life is hushed in repose, is one of wonder and longing to
know more of their being and the hidden causes which brought them forth.
Here, we have poetry written in letters of gold on the sable vestment of
night; music in the gliding motion of the spheres; and harmony in the
orbital sweep of sun, planet, and satellite.

Milton was not only familiar with 'the face of the sky,' as it is
popularly called, but also knew the structure of the celestial sphere,
and the great circles by which it is circumscribed. Two of those--the
colures--he alludes to in the following lines, when he describes the
manner in which Satan, to avoid detection, compassed the Earth, after
his discovery by Gabriel in Paradise, and his flight thence:--

    The space of seven continued nights he rode
    With darkness--thrice the equinoctial line
    He circled, four times crossed the car of night
    From pole to pole, traversing each colure.--ix. 63-66.

Aristarchus of Samos believed the stars were golden studs, that
illumined the crystal dome of heaven; but modern research has
transformed this conception of the ancient astronomer's into a universe
of blazing suns rushing through regions of illimitable space. In
Milton's time astronomers had arrived at no definite conclusion with
regard to the nature of the stars. They were known to be self-luminous
bodies, situated at a remote distance in space, but it had not been
ascertained with any degree of certainty that they were suns, resembling
in magnitude and brilliancy our Sun. Indeed, little was known of those
orbs until within the past hundred years, when the exploration of the
heavens by the aid of greatly increased telescopic power, was the means
of creating a new branch of astronomical science, called sidereal
astronomy.

We are indebted to Sir William Herschel, more than to any other
astronomer, for our knowledge of the stellar universe. It was he who
ascertained the vastness of its dimensions, and attempted to delineate
its structural configuration. He also explored the star depths, which
occupy the infinitude of space by which we are surrounded, and made
many wonderful discoveries, which testify to his ability as an observer,
and to his greatness as an astronomer.

William Herschel was born at Hanover, November 15, 1738. His father was
a musician in the band of the Hanoverian Guard, and trained his son in
his own profession. After four years of military service, young Herschel
arrived in England when nineteen years of age, and maintained himself by
giving lessons in music. We hear of him first at Leeds, where he
followed his profession, and instructed the band of the Durham Militia.
From Leeds he went to Halifax, and was appointed organist there; on the
expiration of twelve months he removed to Bath, and was elected to a
similar post at the Octagon Chapel in that city. Here, fortune smiled
upon him, and he became a busy and prosperous man. Besides attending to
his numerous private engagements, he organised concerts, oratorios, and
other public musical entertainments, which gained him much popularity
among the cultivated classes which frequented this fashionable resort.
Notwithstanding his numerous professional engagements, Herschel was able
to devote a portion of his time to acquiring knowledge on other
subjects. He became proficient in Italian and Greek, studied
mathematics, and read books on astronomy. In 1773 he borrowed a small
telescope, which he used for observational purposes, and was so
captivated with the appearances presented by the celestial bodies, that
he resolved to dedicate his life to acquiring 'a knowledge of the
construction of the heavens.' This resolution he nobly adhered to, and
became one of the most distinguished of astronomers. Like many other
astronomers, Herschel possessed the requisite skill which enabled him to
construct his own telescopes. Being desirous of possessing a more
powerful instrument, and not having the means to purchase one, he
commenced the manufacture of specula, the grinding and polishing of
which had to be done by hand, entailing the necessity of tedious labour
and the exercise of much patience. After repeated failures he at length
completed a 5-1/2-foot Gregorian reflector, and with this instrument
made his first survey of the heavens. Having perceived the desirability
of possessing a more powerful telescope, he equipped himself with a
reflector of twenty feet focal length, and it was with this instrument
that he made those wonderful discoveries which established his
reputation as a great astronomer.

On March 31, 1781, when examining the stars in the constellation Gemini,
Herschel observed a star which presented an appearance slightly
different to that of the other stars by which it was surrounded; it
looked larger, had a perceptible disc, and its light became fainter when
viewed with a higher magnifying power. After having carefully examined
this object, Herschel arrived at the conclusion that he had discovered a
comet. He communicated intelligence of his discovery to the Royal
Society, and, a notification of it having been sent to the Continental
observatories, this celestial visitor was subjected to a close scrutiny;
its progressive motion among the stars was carefully observed, and an
orbit was assigned to it. After it had been under observation for some
time, doubts were expressed as to its being a comet, these were
increased on further examination, and eventually it was discovered that
this interesting object was a new planet. This important discovery at
once raised Herschel to a position of eminence and distinction, and from
a star-gazing musician he became a famous astronomer. A new planet named
Uranus was added to our system, which completes a revolution round the
Sun in a little over eighty-four years, and at a distance of near 1,000
millions of miles beyond the orbit of Saturn. Herschel's name became a
household word. George III. invited him to Court in order that he might
obtain from his own lips an account of his discovery of the new planet;
and so favourable was the impression made by Herschel upon the King,
that he proposed to create him Royal Astronomer at Windsor, and bestow
upon him a salary of 200_l._ a year. Herschel decided to accept the
proffered appointment, and, with his sister Caroline, removed from Bath
to Datchet, near Windsor, in 1782, and from there to Slough in 1786. In
1788 he married the wealthy widow of a London merchant, by whom he had
one son, who worthily sustained his father's high reputation as an
astronomer. Herschel was created a Knight in 1816, and in 1821 was
elected first President of the Royal Astronomical Society. He died at
Slough on August 25, 1822, when in the eighty-fourth year of his age,
and was buried in Upton Churchyard.

It is inscribed on his tomb, that 'he burst the barriers of heaven;' the
lofty praise conveyed by this expression is not greater than what
Herschel merited when we consider with what unwearied assiduity and
patience he laboured to accomplish the results described in the words
which have been quoted. By a method called 'star-gauging' he
accomplished an entire survey of the heavens and examined minutely all
the stars in their groups and aggregations as they passed before his eye
in the field of the telescope. He sounded the depths of the Milky Way,
and explored the wondrous regions of that shining zone, peopled with
myriads of suns so closely aggregated in some of its tracts as to
suggest the appearance of a mosaic of stars. He resolved numerous nebulæ
into clusters of stars, and penetrated with his great telescope depth
after depth of space crowded with 'island universes of stars,' beyond
which he was able to discern luminous haze and filmy streaks of light,
the evidence of the existence of other universes plunged in depths still
more profound, where space verges on infinity. In his exploration of the
starry heavens Herschel's labours were truly amazing. On four different
occasions he completed a survey of the firmament, and counted the stars
in several thousand gauge-fields; he discovered 2,400 nebulæ, 800
double stars, and attempted to ascertain the approximate distances of
the stars by a comparison of their relative brightness.

It had long been surmised, though no actual proof was forthcoming, that
the law of gravitation by which the order and stability of our system
are maintained exercises its potent influence over other material bodies
existing in space, and that other systems, though differing in many
respects from that of ours, and presenting a more complex arrangement in
their structure, perform their motions subject to the guidance of this
universal law. The uncertainty with regard to the controlling influence
of gravity was removed by Herschel when he made his important discovery
of binary star systems. The components of a binary star are usually in
such close proximity that, to the naked eye, they appear as one star,
and sometimes, even with telescopic aid, it is impossible to distinguish
them individually; but when observed with sufficient magnifying power
they can be easily perceived as two lucid points. Double stars were for
a long time believed to be a purely optical phenomenon--an effect
created by two stars projected on the sphere so as to appear nearly in
the same line of vision, and, although apparently almost in contact,
situated at great distances apart. At one time Herschel entertained a
similar opinion with regard to those stars. In 1779 he undertook an
extensive exploration of the heavens with the object of discovering
double stars. As a result of his labours he presented to the Royal
Society in 1782 a list of 269 newly discovered double stars, and in
three years after he supplemented this list with another which contained
434 more new stars. He carefully measured the distances by which the
component stars were separated, and determined their position angles, in
order that he might be able to detect the existence of any sensible
parallax. On repeating his observations twenty years after, he
discovered that the relative positions of many of the stars had changed,
and in 1802 he made the important announcement of his discovery that the
components of many double stars form independent systems, held together
in a mutual bond of union and revolving round one common centre of
gravity.

The importance of this discovery, which we owe to Herschel's sagacity
and accuracy of observation, cannot be over-estimated; what was
previously conjecture and surmise, now became precise knowledge
established upon a sure and accurate basis. It was ascertained that the
law of gravity exerts its power in regulating and controlling the
motions of all celestial bodies within the range of telescopic vision,
and that the order and harmony which pervade our system are equally
present among other systems of suns and worlds distributed throughout
the regions of space. The spectacle of two or more suns revolving round
each other, forming systems of greater magnitude and importance than
that of ours, conveyed to the minds of astronomers a knowledge of the
mechanism of the heavens which had hitherto been unknown to them.

During the many years which Herschel devoted to the exploration of the
starry heavens, and when engaged night after night in examining and
enumerating the various groups and clusters of stars which passed before
his eye in the field of his powerful telescope, he did not fail to
remember the sublime object of his life, and to which he made all his
other investigations subordinate, viz., the delineation of the
structural configuration of the heavens, and the inclusion of all
aggregations, groups, clusters, and galaxies of stars which are
apparently scattered promiscuously throughout the regions of space into
one grand harmonious design of celestial architecture.

Having this object in view, he explored the wondrous zone of the Milky
Way, gauged its depths, measured its dimensions, and, in attempting to
unravel the intricacies of its structure, penetrated its recesses far
beyond the limit attained by any other observer. Acting on the
assumption that the stars are uniformly distributed throughout space,
Herschel, by his method of star-gauging, concluded that the sidereal
system consists of an irregular stratum of evenly distributed suns,
resembling in form a cloven flat disc, and that the apparent richness of
some regions as compared with that of others could be accounted for by
the position from which it was viewed by an observer. The stars would
appear least numerous where the visual line was shortest, and, as it
became lengthened, they would increase in number until, by crowding
behind each other as a greater depth of stratum was penetrated, they
would, when very remote, present the appearance of a luminous cloud or
zone of light. After further observation Herschel was compelled to
relinquish his theory of equal star distribution, and found, as he
approached the Galaxy, that the stars became much more numerous, and
that in the Milky Way itself there was evidence of the gravitation of
stars towards certain regions forming aggregations and clusters which
would ultimately lead to its breaking up into numerous separate sidereal
systems. As he extended his survey of the heavens and examined with
greater minuteness the stellar regions in the Galactic tract, he
discovered that by his method of star-gauging he was unable to define
the complexity of structure and variety of arrangement which came under
his observation; he also perceived that the star-depths are
unfathomable, and discerned that beyond the reach of his telescope there
existed systems and galaxies of stars situated at an appalling distance
in the abysmal depths of space. Though the magnitude of that portion of
the sidereal heavens which came under his observation was inconceivable
as regards its dimensions, Herschel was able to perceive that it formed
but a part--and most probably a small part--of the stellar universe, and
that without a more extended knowledge of this universe, which at
present is unattainable, it would be impossible to determine its
structural configuration or discover the relationships that exist among
the sidereal systems and Galactic concourses of stars distributed
throughout space. Herschel ultimately abandoned his star-gauging method
of observation and confined his attention to exploring the star depths
and investigating the laws and theories associated with the bodies
occupying those distant regions.

Since all the planets if viewed from the Sun would be seen to move
harmoniously and in regular order round that body, so there may be
somewhere in the universe a central point, or, as some persons imagine,
a great central sun, round which all the systems of stars perform their
majestic revolutions with the same beautiful regularity; having their
motions controlled by the same law of gravitation, and possessing the
same dynamical stability which characterises the mechanism of the solar
system.

The extent of the distance which intervenes between our system and the
fixed stars constituted a problem which exercised the minds of
astronomers from an early period until the middle of the present
century.

Tycho Brahé, who repudiated the Copernican theory, asserted as one of
his reasons against it that the distances by which the heavenly bodies
are separated from each other were greater than even the upholders of
this theory believed them to be. Although the distance of the Sun from
the Earth was unknown, Tycho was aware that the diameter of the Earth's
orbit must be measured by millions of miles, and yet there was no
perceptible motion or change of position of the stars when viewed from
any point of the vast circumference which she traverses. Consequently,
the Earth, if viewed from the neighbourhood of a star, would also appear
motionless, and the dimensions of her orbit would be reduced to that of
a point. This seemed incredible to Tycho, and he therefore concluded
that the Copernican theory was incorrect.

The conclusion that the stars are orbs resembling our Sun in magnitude
and brilliancy was one which, Tycho urged, should not be hastily
adopted; and yet, if it were conceded that the Earth is a body which
revolves round the Sun, it would be necessary to admit that the stars
are suns also. If the Earth's orbit, as seen from a star, were reduced
to a point, then the Sun, which occupies its centre, would be reduced to
a point of light also, and, when observed from a star of equal
brilliancy and magnitude, would have the same resemblance that the star
has when viewed from the Earth, which may be regarded as being in
proximity to the Sun. Tycho Brahé would not admit the accuracy of these
conclusions, which were too bewildering and overwhelming for his mental
conception.

But the investigations of later astronomers disclosed the fact that the
heavenly bodies are situated at distances more remote from each other
than had been previously imagined, and that the reasons which led Tycho
to reject the Copernican theory were based upon erroneous conclusions,
and could, with greater aptitude, be employed in its support. It was
ascertained that the distance of the Sun from the Earth, which at
different periods was surmised to be ten, twenty, and forty millions of
miles, was much greater than had been previously estimated. Later
calculations determined it to be not less than eighty millions of miles,
and, according to the most recent observations, the distance of the Sun
from the Earth is believed to be about ninety-three millions of miles.

Having once ascertained the distance between the Earth and the Sun,
astronomers were enabled to determine with greater facility the
distances of other heavenly bodies.

It was now known that the diameter of the Earth's orbit exceeded 183
millions of miles, and yet, with a base line of such enormous length,
and with instruments of the most perfect construction, astronomers were
only able to perceive the minutest appreciable alteration in the
positions of a few stars when observed from opposite points of the
terrestrial orbit.

It had long been the ambitious desire of astronomers to accomplish, if
possible, a measurement of the abyss which separates our system from the
nearest of the fixed stars. No imaginary measuring line had ever been
stretched across this region of space, nor had its unfathomed depths
ever been sounded by any effort of the human mind. The stars were known
to be inconceivably remote, but how far away no person could tell, nor
did there exist any guide by which an approximation of their distances
could be arrived at.

In attempting to calculate the distances of the stars, astronomers have
had recourse to a method called 'Parallax,' by which is meant the
apparent change of position of a heavenly body when viewed from two
different points of observation.

The annual parallax of a heavenly body is the angle subtended at that
body by the radius of the Earth's orbit.

The stars have no diurnal parallax, because, owing to their great
distance, the Earth's radius does not subtend any measurable angle, but
the radius of the Earth's orbit, which is immensely larger, does, in the
case of a few stars, subtend a very minute angle.

'This enormous base line of 183 millions of miles is barely sufficient,
in conjunction with the use of the most delicate and powerful
astronomical instruments, to exhibit the minutest measureable
displacement of two or three of the nearest stars.'--Proctor.

The efforts of early astronomers to detect any perceptible alteration in
the positions of the stars when observed from any point of the
circumference of the Earth's orbit were unsuccessful. Copernicus
ascribed the absence of any parallax to the immense distances of the
stars as compared with the dimensions of the terrestrial orbit. Tycho
Brahé, though possessing better appliances, and instruments of more
perfect construction, was unable to perceive any annual displacement of
the stars, and brought this forward as evidence against the Copernican
theory.

Galileo suggested a method of obtaining the parallax of the fixed stars,
by observing two stars of unequal magnitude apparently near to each
other, though really far apart. Those, when observed from different
points of the Earth's orbit, would appear to change their positions
relatively to each other. The smaller and more distant star would remain
unaltered, whilst the larger and nearer star would have changed its
position with respect to the other. By continuing to observe the larger
star during the time that the Earth accomplished a revolution of her
orbit, Galileo believed that its parallax might be successfully
determined. Though he did not himself put this method into practice, it
has been tried by others with successful results.

In 1669, Hooke made the first attempt to ascertain the parallax of a
fixed star, and selected for this purpose Gamma Draconis, a bright star
in the Head of the Dragon. This constellation passed near the zenith of
London at the time that he made his observations, and was favourably
situated, so as to avoid the effects of refraction. Hooke made four
observations in the months of July, August, and October, and believed
that he determined the parallax of the star; but it was afterwards
discovered that he was in error, and that the apparent displacement of
the star was mainly due to the aberration of light--a phenomenon which
was not discovered at that time.

A few years later, Picard, a French astronomer, attempted to find the
parallax of Alpha Lyræ, but was unsuccessful. In 1692-93, Roemer, a
Danish astronomer, observed irregularities in the declinations of the
stars which could neither be ascribed to parallax or refraction, and
which he imagined resulted from a changing position of the Earth's axis.

One of the principal causes which baffled astronomers in their
endeavours to determine the parallax of the fixed stars was a phenomenon
called the 'Aberration of Light,' which was discovered and explained by
Bradley in 1727. The peculiar effect of aberration was perceived by him
when endeavouring to obtain the parallax of Gamma Draconis.

Owing to the progressive transmission of light, conjointly with the
motion of the Earth in her orbit, there results an apparent slight
displacement of a star from its true position. The extent of the
displacement depends upon the ratio of the velocity of light as compared
with the speed of the Earth in her orbit, which is as 10,000 to 1. As a
consequence of this, each star describes a small ellipse in the course
of a year, the central point of which would indicate the place occupied
by the star if the Earth were at rest. The shifting position of the star
is very slight, and at the end of a year it returns to its former place.

Prior to the discovery of aberration, astronomers ascribed the apparent
displacement of the stars arising from this cause as being due to
parallax--a conclusion which led to erroneous results; but after
Bradley's discovery this source of error was avoided, and it was found
that the parallax of the stars had to be considerably reduced.

Bessel was the first astronomer who merited the high distinction of
having determined the first reliable stellar parallax, and by this
achievement he was enabled to fathom the profound abyss which separates
our solar system from the stars.

Frederick William Bessel was born in 1764 at Minden, in Westphalia. It
was his intention to pursue a mercantile career, and he commenced life
by becoming apprenticed to a firm of merchants at Bremen. Soon
afterwards he accompanied a trading expedition to China and the East
Indies, and while on this voyage picked up a good deal of information
with regard to many matters which came under his observation. He
acquired a knowledge of Spanish and English, and made himself acquainted
with the art of navigation. On his return home, Bessel endeavoured to
determine the longitude of Bremen. The only appliances which he made use
of were a sextant constructed by himself, and a common clock; and yet,
with those rude instruments, he successfully accomplished his object.
During the next two years he devoted all his spare time to the study of
mathematics and astronomy, and, having obtained possession of Harriot's
observations of the celebrated comet of 1607--known as Halley's
comet--Bessel, after much diligent application and careful calculation,
was enabled to deduce from them an orbit, which he assigned to that
remarkable body. This meritorious achievement was the means of procuring
for him a widely known reputation.

A vacancy for an assistant having occurred at Schröter's Observatory at
Lilienthal, the post was offered to Bessel and accepted by him. Here he
remained for four years, and was afterwards appointed Director of the
new Prussian Observatory at Königsberg, where he pursued his
astronomical labours for a period of upwards of thirty years. Bessel
directed his energies chiefly to the study of stellar astronomy, and
made many observations in determining the number, the exact positions,
and proper motions of the stars. He was remarkable for the precision
with which he carried out his observations, and for the accuracy which
characterised all his calculations.

In 1837 Bessel, by the exercise of his consummate skill, endeavoured to
solve a problem which for many years baffled the efforts of the ablest
astronomers, viz., the determination of the parallax of the fixed stars.
This had been so frequently attempted, and without success, that the
results of any new observations were received with incredulity before
their value could be ascertained.

Bessel was ably assisted by Joseph Frauenhofer, an eminent optician of
Munich, who constructed a magnificent heliometer for the Observatory at
Königsberg, and in its design introduced a principle which admirably
adapted it for micrometrical measurement.

The star selected by Bessel is a binary known as 61 Cygni, the
components being of magnitudes 5·5 and 6 respectively. It has a large
proper motion, which led him to conclude that its parallax must be
considerable.

This star will always be an object of interest to astronomers, as it was
the first of the stellar multitude that revealed to Bessel the secret of
its distance.

Bessel commenced his observations in October 1837, and continued them
until March 1840. During this time he made 402 measurements, and, before
arriving at a conclusive result, carefully considered every imaginable
cause of error, and rigorously calculated any inaccuracies that might
arise therefrom. Finally, he determined the parallax of the star to be
0´´·3483--a result equivalent to a distance about 600,000 times that of
the Earth from the Sun. In 1842-43 M. Peters, of the Pulkova
Observatory, arrived at an almost similar result, having obtained a
parallax of 0´´·349; but by more recent observations the parallax of the
star has been increased to about half a second.

About the same time that Bessel was occupied with his observation of 61
Cygni, Professor Henderson, of Edinburgh, when in charge of the
Observatory at the Cape of Good Hope, directed his attention to Alpha
Centauri, one of the brightest stars in the Southern Hemisphere. During
1832-33 he made a series of observations of the star, with the object
of ascertaining its mean declination; and, having been informed
afterwards of its large proper motion, he resolved to make an endeavour
to determine its parallax. This he accomplished after his return to
Scotland, having been appointed Astronomer Royal in that country. By an
examination of the observations made by him at the Cape, he determined
the parallax of Alpha Centauri to be 1´´·16, but later astronomers have
reduced it to 0´´·75.

Professor Henderson's detection of the parallax of Alpha Centauri was
communicated to the Astronomical Society two months after Bessel
announced his determination of the parallax of 61 Cygni.

The parallax of 61 Cygni assigns to the star a distance of forty
billions of miles from the Earth, and that of Alpha Centauri--regarded
as the nearest star to our system--a distance of twenty-five billions of
miles.

It is utterly beyond the capacity of the human mind to form any adequate
conception of those vast distances, even when measured by the velocity
with which the ether of space is thrilled into light. Light, which
travels twelve millions of miles in a minute, requires 4-1/3 years to
cross the abyss which intervenes between Alpha Centauri and the Earth,
and from 61 Cygni the period required for light to reach our globe is
rather less than double that time.

The parallax of more than a dozen other stars has been determined, and
the light passage of a few of the best known is estimated as
follows:--Sirius, eight years; Procyon, twelve; Altair, sixteen;
Aldebaran, twenty-eight; Capella, thirty; Regulus, thirty-five; Polaris,
sixty-three; and Vega, ninety-six years.

It does not always follow that the brightest stars are those situated
nearest to our system, though in a general way this may be regarded as
correct. The diminishing magnitudes of the stars can be accounted for
mainly by their increased distances, rather than by any difference in
their intrinsic brilliancy. We should not err by inferring that the most
minute stars are also the most remote; the telescope revealing thousands
that are invisible to the naked eye. There are, however, exceptions to
this general rule, and there are many stars of small magnitude less
remote than those whose names have been enumerated, and whose light
passage testifies to their profound distances and surpassing magnitude
when compared with that of our Sun.

Sirius, 'the leader of the heavenly host,' is distant fifty billions of
miles. The orb shines with a brilliancy far surpassing that of the Sun,
and greatly exceeds him in mass and dimensions. Arcturus, the bright
star in Boötes, whose golden yellow light renders it such a conspicuous
object, is so far distant that its measurement gives no reliable
parallax; and if we may infer from what little we know of the stars,
Arcturus is believed to be the most magnificent and massive orb entering
into the structure of that portion of the sidereal system which comes
within our cognisance. Judging by its relative size and brightness,
this star is ten thousand times more luminous, and may exceed the Sun
one million times in volume.

Deneb, in the constellation of the Swan, though a first-magnitude star,
possesses no perceptible proper motion or parallax--a circumstance
indicative of amazing distance, and magnitude equalling, or surpassing,
Arcturus and Sirius.

Canopus, in the constellation Argo, in the Southern Hemisphere, the
brightest star in the heavens with the exception of Sirius, possesses no
sensible parallax; consequently, its distance is unknown, though it has
been estimated that its light passage cannot be less than sixty-five
years.

By establishing a mean value for the parallax of stars of different
magnitudes, it was believed that an approximation of their distances
could be obtained by calculating the time occupied in their light
passage. The light period for stars of the first magnitude has been
estimated at thirty-six and a half years; this applies to the brightest
stars, which are also regarded as the nearest. At the distance indicated
by this period, the Sun would shrink to the dimensions of a
seventh-magnitude star and become invisible to the naked eye; this of
itself affords sufficient proof that the great luminary of our system
cannot be regarded as one of the leading orbs of the firmament. Stars of
the second magnitude have a mean distance of fifty-eight light years,
those of the third magnitude ninety-two years, and so on. M. Peters
estimated that light from stars of the sixth magnitude, which are just
visible to the naked eye, requires a period of 138 years to accomplish
its journey hither; whilst light emitted from the smallest stars visible
in large telescopes does not reach the Earth until after the lapse of
thousands of years from the time of leaving its source.

The profound distances of the nearest stars by which we are surrounded
lead us to consider the isolated position of the solar system in space.
A pinnacle of rock, or forsaken raft floating in mid-ocean, is not more
distant from the shore than is the Sun from his nearest neighbours. The
inconceivable dimensions of the abyss by which the orb and his
attendants are surrounded in utter loneliness may be partially
comprehended when it is known that light, which travels from the Sun to
the Earth--a distance of ninety-three millions of miles--in eight
minutes, requires a period of four and a third years to reach us from
the nearest fixed star. A sphere having the Sun at its centre and this
nearest star at its circumference would have a diameter of upwards of
fifty billions of miles; the volume of the orb when compared with the
dimensions of this circular vacuity of space is as a small shot to a
globe 900 miles in diameter. It has been estimated by Father Secchi
that, if a comet when at aphelion were to arrive at a point midway
between the Sun and the nearest fixed star, it would require one hundred
million years in the accomplishment of its journey thither. And yet the
Sun is one of a group of stars which occupy a region of the heavens
adjacent to the Milky Way and surrounded by that zone; nor is his
isolation greater than that of those stars which are his companions, and
who, notwithstanding their profound distance, influence his movements by
their gravitational attraction, and in combination with the other stars
of the firmament control his destiny.

Ancient astronomers, for the purpose of description, have mapped out the
heavens into numerous irregular divisions called 'constellations.' They
are of various forms and sizes, according to the configuration of the
stars which occupy them, and have been named after different animals,
mythological heroes, and other objects which they appear to resemble. In
a few instances there does exist a similitude to the object after which
a constellation is called; this is evident in the case of Corona
Borealis (the Northern Crown), in which there can be seen a conspicuous
arrangement of stars resembling a coronet, and in the constellations of
the Dolphin and Scorpion, where the stars are so distributed that the
forms of those creatures can be readily recognised. There is some slight
resemblance to a bear in Ursa Major, and to a lion in Leo, and no great
effort of the mind is required to imagine a chair in Cassiopeia, and a
giant in Orion; but in the majority of instances it is difficult to
perceive any likeness of the object after which a constellation is
named, and in many cases there is no resemblance whatever.

The constellations are sixty-seven in number: excluding those of the
Zodiac, which have been already mentioned, the constellations of the
Northern Hemisphere number twenty-nine. The most important of these are
Ursa Major and Minor, Andromeda, Cassiopeia, Cepheus, Cygnus, Lyra,
Aquila, Auriga, Draco, Boötes, Hercules, Pegasus, and Corona Borealis.

To an observer of the nocturnal sky the stars appear to be very
unequally distributed over the celestial sphere. In some regions they
are few in number and of small magnitude, whilst in other parts of the
heavens, and especially in the vicinity of the Milky Way, they are
present in great numbers and form groups and aggregations of striking
appearance and conspicuous brilliancy. On taking a casual glance at the
midnight sky on a clear moonless night, one is struck with the apparent
countless multitude of the stars; yet this impression of their vast
number is deceptive, for not more than two thousand stars are usually
visible at one time.

Much, however, depends upon the keenness of vision of the observer, and
the transparency of the atmosphere. Argelander counted at Bonn more than
3,000 stars, and Hozeau, near the equator, where all the stars of the
sphere successively appear in view, enumerated 6,000 stars. This number
may be regarded as including all the stars in the heavens that are
visible to the naked eye. With the aid of an opera glass thousands of
stars can be seen that are imperceptible to ordinary vision.
Argelander, with a small telescope of 2-1/2 inches aperture, was able to
count 234,000 stars in the Northern Hemisphere. Large telescopes reveal
multitudes of stars utterly beyond the power of enumeration, nor do they
appear to diminish in number as depth after depth of space is penetrated
by powerful instruments. The star-population of the heavens has been
reckoned at 100,000,000, but this estimate is merely an assumption;
recent discoveries made by means of stellar photography indicate that
the stars exist in myriads. It is reasonable to believe that there is a
limit to the sidereal universe, but it is impossible to assign its
bounds or comprehend the apparently infinite extent of its dimensions.

Scintillation or twinkling of the stars is a property which
distinguishes them from the planets. It is due to a disturbed condition
of the atmosphere and is most apparent when a star is near the horizon;
at the zenith it almost entirely vanishes. Humboldt states that in the
clear air of Cumana, in South America, the stars do not twinkle after
they reach an elevation of 15° above the horizon. The presence of
moisture in the atmosphere intensifies scintillation, and this is
usually regarded as a prognostication of rain. White stars twinkle more
than red ones. The occurrence of scintillation can be accounted for by
the fact that the stars are visible as single points of light which
twinkle as a whole, but in the case of the Sun, Moon, and planets, they
form discs from which many points of light are emitted; they,
therefore, do not scintillate as a whole, for the absence of rays of
light from one portion of their surface is compensated by those from
other parts of their discs, giving a mean average which creates a
steadiness of vision.

The stars are divided into separate classes called 'magnitudes,' by
which their relative apparent size and degree of brightness are
distinguished. The magnitude of a star does not indicate its mass or
dimensions, but its light-giving power, which depends partly upon its
size and distance, though mainly upon the intensity of its luminosity.
The most conspicuous are termed stars of the first magnitude; there are
ten of those in the Northern Hemisphere, and an equal number south of
the equator, but they are not all of the same brilliancy. Sirius
outshines every other star of the firmament, and Arcturus has no rival
in the northern heavens. The names of the first-magnitude stars north of
the equator are: Arcturus, Capella, Vega, Betelgeux, Procyon, Aldebaran,
Altair, Pollux, Regulus, and Deneb. The next class in order of
brightness are called second-magnitude stars; they are fifty or sixty in
number, the most important of which is the Pole Star. The stars diminish
in luminosity by successive gradations, and when they sink to the sixth
magnitude reach the utmost limit at which they appear visible to the
naked eye. In great telescopes this classification is carried so low as
to include stars of the eighteenth and twentieth magnitudes.

Entering into the structure of the stellar universe we have Single
Stars, Double Stars, Triple, Quadruple, and Multiple Stars, Temporary,
Periodical, and Variable Stars, Star-groups, Star-clusters, Galaxies,
and Nebulæ.

SINGLE OR INSULATED STARS include all those orbs sufficiently isolated
in space so as not to be perceptibly influenced by the attraction of
other similar bodies. They are believed to constitute the centres of
planetary systems, and fulfil the purpose for which they were created by
dispensing light and heat to the worlds which circle around them.

The Sun is an example of this class of star, and constitutes the centre
of the system to which the Earth belongs. Reasoning from analogy, it
would be natural to conclude that there are other suns, numberless
beyond conception, the centres of systems of revolving worlds, and
although we are utterly unable to catch a glimpse of their planetary
attendants, even with the aid of the most powerful telescopes, yet they
have in a few instances been _felt_, and have afforded unmistakable
indications of their existence.

Since the Sun must be regarded as one of the stellar multitude that
people the regions of space, and whose surpassing splendour when
contrasted with that of other luminaries can be accounted for by his
proximity to us, it would be of interest to ascertain his relative
importance when compared with other celestial orbs which may be his
peers or his superiors in magnitude and brilliancy.

The Sun is one of a widely scattered group of stars situated in the
plane of the Milky Way and surrounded by that zone, and, as a star among
the stars, would be included in the constellation of the Centaur.

Although regarded as one of the leading orbs of the firmament, and of
supreme importance to us, astronomers are undecided whether to classify
the Sun with stars of greater magnitude and brightness, or assign him a
position among minor orbs of smaller size. Much uncertainty exists with
regard to star magnitudes. This arises from inability on the part of
astronomers to ascertain the distances of the vast majority of stars
visible to the naked eye, and also on account of inequality in their
intrinsic brilliancy. Among the stars there exists an indefinite range
of stellar magnitudes. There are many stars known whose dimensions have
been ascertained to greatly exceed those of the Sun, and there are
others of much smaller size. No approximation of the magnitude of
telescopic stars can be arrived at; many of them may rival Sirius,
Canopus, and Arcturus, in size and splendour, their apparent minuteness
being a consequence of their extreme remoteness. If the Sun were removed
a distance in space equal to that of many of the brightest stars, he
would in appearance be reduced to a minute point of light or become
altogether invisible; and there are other stars, situated at distances
still more remote, of which sufficient is known to justify us in
arriving at the conclusion that the Sun must be ranked among the minor
orbs of the firmament, and that many of the stars surpass him in
brilliancy and magnitude.

DOUBLE STARS.--To the unaided eye, these appear as single points of
light; but, when observed with a telescope of sufficient magnifying
power, their dual nature can be detected.

The first double star discovered was Mizar, the middle star of the three
in Ursa Major which form the tail of the bear. The components are of the
fourth and fifth magnitudes, of a brilliant white colour, and distant
fourteen seconds of arc.

In 1678, Cassini perceived stars which appeared as single points of
light when viewed with the naked eye, but when observed with the
telescope presented the appearance of being double.

The astronomer Bode, in 1781, published a list of eighty double stars,
and, in a few years after, Sir William Herschel discovered several
hundreds more of those objects. They are now known to exist in
thousands, Mr. Burnham, of the Lick Observatory, having, by his keen
perception of vision, contributed more than any other observer to swell
their number.

All double stars are not binaries; many of them are known as 'optical
doubles'--an impression created by two stars when almost in the same
line of vision, and, though apparently near, are situated at a great
distance apart and devoid of any physical relationship.

Binary stars consist of two suns which revolve round their common
centre of gravity, and form real dual systems.

The close proximity of the components of double stars impressed the
minds of some astronomers with the belief that a physical bond of union
existed between them. In the interval between 1718 and 1759, Bradley
detected a change of 30° in the position angle of the two stars forming
Castor, and was very nearly discovering their physical connection.

In 1767, the Rev. John Michell wrote: 'It is highly probable in
particular, and next to a certainty in general, that such double stars
as appear to consist of two or more stars placed very near together do
really consist of stars placed near together and under the influence of
some general law.' Afterwards he says: 'It is not improbable that a few
years may inform us that some of the great number of double and triple
stars which have been observed by Mr. Herschel are systems of bodies
revolving about each other.' Christian Mayer, a German astronomer,
formed a list of stellar pairs, and announced, in 1776, the supposed
discovery of 'satellites' to many of the principal stars. His
observations were, however, not exact enough to lead to any useful
results, and the existence of his 'planet stars' was at that time
derided, and believed to find a place only in his imagination.

The conclusions arrived at by some astronomers with regard to double
stars were afterwards confirmed by Herschel, when, by his observation of
a change in the relative positions of many of their components, he was
able to announce that they form independent systems in mutual
revolution, and are controlled by the law of gravitation.

The number of binary stars in active revolution is known to exceed 500;
but, besides these, there are doubtless numerous other compound stars
which, on account of their extreme remoteness and the close proximity of
their components, are irresolvable into pairs by any optical appliances
which we possess.

The revolution of two suns in one sphere presents to our observation a
scheme of creative design entirely different to the single-star system
with which we are familiar--one of a higher and more complex order in
the ascending scale of celestial architecture. For, if we assume that
around each revolving sun there circles a retinue of planetary worlds,
it is obvious that a much more complicated arrangement must exist among
the orbs which enter into the formation of such a system than is found
among those which gravitate round our Sun.

The common centre of gravity of a binary system is situated on a line
between both stars, and distant from each in inverse proportion to their
respective masses. When the stars are of equal mass their orbits are of
equal dimensions, but when the mass of one star exceeds that of the
other, the orbit of the larger star is proportionately diminished as
compared with the circumference traversed by the smaller star. When
their orbits are circular--a rare occurrence--both stars pursue each
other in the same path, and invariably occupy it at diametrically
opposite points; nor is it possible for one star to approach the other
by the minutest interval of space in any duration of time, so long as
the synchronous harmony of their revolution remains undisturbed.

[Illustration: FIG. 3.--A Binary Star System--70 Ophiuchi

(_Drawn by Mr. J. E. Gore._)]

When a pair of suns move in an ellipse, their orbits intersect and are
of equal dimensions when the stars are of equal mass, their common
centre of gravity being then at a point equidistant from each.
Consequently, neither star can approach or recede from this point
without the other affecting a similar motion, they must be at periastron
and apastron together, and any acceleration or retardation of speed must
occur simultaneously with each. Stars of unequal magnitude always
maintain a proportionate distance from their common focus, and both
simultaneously occupy corresponding parts of their orbits.

The nature of the motions of those distant suns, and the form of the
orbits which they traverse, have been investigated by several eminent
astronomers, and although the subject is one of much difficulty, on
account of their extreme remoteness and the minute angles which have to
be dealt with, necessitating the carrying out of very refined
observations, yet a considerable amount of information has been obtained
with regard to the paths which they pursue in the accomplishment of
their revolutions round each other.

The orbits of about sixty stellar pairs have been computed, but only
with partial success. Some stars have shown themselves to be totally
regardless of theory and computation, and have shot ahead far beyond the
limits ascribed to them, whilst others, by the slowness of their
motions, have upset the calculations of astronomers as much in the
opposite direction. So that out of this number the orbits of not more
than half a dozen are satisfactorily known.

The dimensions of stellar orbits are of very varied extent. Some pairs
are apparently so close that the best optical means which we possess are
incapable of dividing them, whilst others revolve in wide and spacious
orbits.

The most marked peculiarity of the orbits of binary stars is their high
eccentricity; they are usually much more eccentric than are those of
the planets, and in some instances approach in form that of a comet.

The finest binary star in the northern heavens is Castor, the brighter
of the two leading stars in the constellation Gemini. The components are
of the second and third magnitudes, and over five seconds apart. They
are of a brilliant white colour, and form a beautiful object in the
telescope.

In 1719 Bradley determined the relative positions of those stars, and on
comparing the results obtained by him with recent measurements it was
found that they had altered to the extent of 125°. Travelling at the
same rate of speed, they will require a period of about 420 years to
complete an entire circuit of their orbits. This pace, however, has not
been maintained, for, their periastron having occurred in 1750, they
travelled more rapidly in the last century than they are doing at
present, and, as their orbits are so eccentric that when at apastron the
stars are twice as remote from each other as at periastron, they will
for the next three and a half centuries continue to slacken their pace,
until they shall have reached the most remote points of their orbits,
when they will again begin to approach with an increasing velocity; so
that the time in which an entire revolution can be accomplished will not
be much less than 1,000 years.[8]

As the distance of Castor is unknown, it is impossible to compute the
combined mass of its components. They are very remote, their light
period being estimated at forty-four years. Castor is doubtless a more
massive orb than our Sun, and possesses a higher degree of luminosity.

Alpha Centauri, in the Southern Hemisphere, is the brightest binary, and
also the nearest known star in the heavens; its estimated distance being
twenty-five billions of miles. Both components equal stars of the first
magnitude, and are of a brilliant white colour. Since they were first
observed, in 1709, they have completed two revolutions, and are now
accomplishing a third. The eccentricity of their orbit approaches in
form that of Faye's comet, which travels round the Sun; consequently the
stars, when at apastron, are twice their periastron distance. Their
period of revolution is about eighty-eight years. The mean radius of
their orbit corresponds to a span of 1,000 millions of miles, so that
those orbs are sometimes as close to each other as Jupiter is to the
Sun, and never so far distant as Uranus.[9] Their combined mass is twice
that of the Sun, and the luminosity of each star is slightly greater.

The double star 61 Cygni--one of the nearest to our system--is believed
to be a binary the components of which move in an orbit of more spacious
dimensions than that of any other known revolving pair. Though they have
been under continuous observation since 1753, it is only within the last
few years that any orbital motion has been perceived. Some observers
are disinclined to admit the accuracy of this statement; whilst others
believe that the stars have executed a hyperbolic sweep round their
common centre of gravity and are now separating.

The radius of the orbit in which those bodies travel is sixty-five times
the distance of the Earth from the Sun; which means that they travel in
an orbit twice the width of that of the planet Neptune. It has been
estimated that they complete a revolution in about eight centuries. The
united mass of the system is about one-half that of the Sun, and in
point of luminosity they are much inferior to that orb.

The star 70 Ophiuchi (fig. 3) may be regarded as typical of a binary
system. The components are five seconds apart, and of the fourth and
sixth magnitudes. Their light period is stated to be twenty years, and
the combined mass of the system is nearly three times that of the Sun.
The pair travel in an orbit from fourteen to forty-two times the radius
of the Earth's orbit; so that when at apastron they are three times as
distant from each other as when at periastron. They complete a
revolution in eighty-eight years.

The accompanying diagram (fig. 4) is a delineation of the beautiful
orbits of the components of Gamma Virginis. These may be described as
elongated ellipses. Both stars being of equal mass, their orbits are of
equal dimensions, and their common centre of gravity at a point
equidistant from each. Any approach to, or recession from this point,
must occur simultaneously with each; they must always occupy
corresponding parts of their orbits, and be in apastron and at
periastron in the same period of time. The ellipse described by this
pair is the most eccentric of known binary orbits, and approaches in
form the path pursued by Encke's comet round the Sun. These orbs
complete a revolution in 180 years, and when in apastron are seventeen
times more remote from each other than when at periastron.

[Illustration: FIG. 4.--The Orbits of the Components of Gamma Virginis.]

From his observation of the motion of Sirius in 1844, Bessel was led to
believe that the brilliant orb was accompanied by another body, whose
gravitational attraction was responsible for the irregularities observed
in the path of the great dog-star when pursuing his journey through
space. The elements of this hypothetical body were afterwards computed
by Peters and Auwers, and its exact position assigned by Safford in
1861.

On January 31, 1862, Mr. Alvan Clarke, of Cambridgeport, Massachusetts,
when engaged in testing a recently constructed telescope of great power,
directed it on Sirius, and was enabled by good fortune to discover the
companion star at a distance of ten seconds from its primary. Since its
discovery, the star has pursued with such precision the theoretical path
previously assigned to it that astronomers have had no hesitation in
identifying it as the hypothetical body whose existence Bessel had
correctly surmised.

[Illustration: FIG. 5.--Apparent Orbit of the Companion of Sirius.

(_Drawn by Mr. Burnham._)]

The Sirian satellite is a yellow star of the eighth magnitude, and
shines with a feeble light when contrasted with the surpassing
brilliancy of its neighbour.

Astronomers were for some time in doubt as to whether the uneven motion
which characterised the path of Sirius could be ascribed to the
attraction of its obscure attendant, which presented such a marked
contrast to its primary, and several observers were inclined to believe
that the disturbing body still remained undiscovered. When, however, the
density of the lesser star became known, it was discovered that, weight
for weight, that of Sirius exceeded it only in the proportion of two to
one, though as a light-giver the great orb is believed to be 5,000 times
more luminous. The Sirian satellite revolves round its primary in about
fifty years, and at a distance twenty-eight times that of the Earth from
the Sun.

The surpassing brilliancy of Sirius as compared with that of the other
stars of the firmament has rendered it at all times an object of
interest to observers. The Egyptians worshipped the star as Sothis, and
it was believed to be the abode of the soul of Isis. The nations
inhabiting the region of the Nile commenced their year with the heliacal
rising of Sirius, and its appearance was regarded as a sure forerunner
of the rising of the great river, the fertilising flood of which was
attributed to the influence of this beautiful star. It is believed that
the Mazzaroth in Job is an allusion to this brilliant orb. Among the
Romans Sirius was regarded as a star of evil omen; its appearance above
the horizon after the summer solstice was believed to be associated with
pestilence and fevers, consequent upon the oppressive heat of the
season of the year. The _dies caniculares_, or dog-days, were reckoned
to begin twenty days before, and to continue for twenty days after, the
heliacal rising of Sirius, the dog-star. During those days a peculiar
influence was believed to exist which created diseases in men and
madness among dogs. Homer alludes to the star

                                'whose burning breath
    Taints the red air with fevers, plagues and death.'

Sirius, which is in Canis Major (one of Orion's hunting dogs), is a far
more glorious orb than our Sun. According to recent photometric
measurements it emits seventy times the quantity of light, and is three
times more massive than the great luminary of our system. At the
distance of Sirius (fifty billions of miles) the Sun would shrink to the
dimensions of a third-magnitude star, and the light of seventy such
stars would be required to equal in appearance the brilliant radiance of
the great dog-star. The orb, with his retinue of attendant worlds--some
of which are reported as having been seen--is travelling through space
with a velocity of not less than 1,000 miles a minute.

An irregularity of motion resembling that of Sirius has been detected
with regard to Procyon, the lesser dog-star. But in this case the
companion star has not as yet been seen, though a careful search has
been made for it with the most powerful of telescopes. Should it be a
planetary body, illumined by its primary, its reflected light would not
appear visible to us, even if it were much less remote than it is.

We are able only to perceive the effulgence of brilliant suns scattered
throughout the regions of space; but besides those, there are doubtless
many faintly luminous orbs and opaque bodies of vast dimensions
occupying regions unknown to us, but by a knowledge of the existence of
which an enlarged conception is conveyed to our minds of the greatness
of the universe.

The most rapid of known revolving pairs is Delta Equulei. The components
are so close that only the finest instruments can separate them, and
this they cannot do at all times. They accomplish a revolution in eleven
and a half years. The slowest revolving pair is Zeta Aquarii. The motion
of the components is so tardy that to complete a circuit of their orbits
they require a period of about sixteen centuries. Other binary stars
have had different periods assigned to them; eleven pairs have been
computed to revolve round each other in less than fifty years, and
fifteen in less than 100 but more than fifty. There are other compound
stars whose motions appear to be much more leisurely than those just
mentioned, and although no orbital movement has, so far, been detected
among them, yet, so vast is the scale upon which the sidereal system is
constructed, that thousands of years must elapse before they can have
accomplished a revolution of their orbits.

The Pole Star is an optical double, but the components are of very
unequal magnitude. The Pole Star itself is of the second magnitude, but
its companion is only of the ninth, and on account of its minuteness is
regarded as a good test for telescopes of small aperture. Mizar, in the
constellation Ursa Major, is a beautiful double star. The components are
wide apart, and can be easily observed with a small instrument.

There is a remarkable star in the constellation of the Lyre (Epsilon
Lyræ), described as a double double. This object can just be
distinguished by a person with keen eyesight as consisting of two stars;
when observed with a telescope they appear widely separated, and each
star is seen to have a companion, the entire system forming two binary
pairs in active revolution. The pair which first cross the meridian
complete a revolution in about 2,000 years; the second pair have a more
rapid motion, and accomplish it in half that time. The two pairs are
believed to be physically connected, and revolve round their common
centre of gravity in a period of time not much under one million years.

Cor Caroli, in Canes Venatici, is a pleasing double star, the components
being of a pale white and lilac colour.

Albireo, in the constellation of the Swan, is one of the loveliest of
double stars. The larger component is of the third magnitude, and of a
golden yellow colour; the smaller of the sixth magnitude, and of a
sapphire blue.

Epsilon Boötis, known also as Mirac, and called by Admiral Smyth
'Pulcherrima,' on account of its surpassing beauty, is a delicate object
of charming appearance. The components of this lovely star are of the
third and seventh magnitudes: the primary orange, the secondary
sea-green.

The late Mr. R. A. Proctor, in describing a binary star system, writes
as follows: 'If we regard a pair of stars as forming a double sun, round
which--or, rather, round the common centre of which--other orbs revolve
as planets, we are struck by the difference between such a scheme and
our own solar system; but we find the difference yet more surprising
when we consider the possibility that in some such schemes each
component sun may have its own distinct system of dependent worlds. In
the former case the ordinary state of things would probably be such that
both suns would be above the horizon at the same time, and then,
probably, their distinctive peculiarities would only be recognisable
when one chanced to pass over the disc of the other, as our Moon passes
over the Sun's disc in eclipses. For short intervals of time, however,
at rising or setting, one or other would be visible alone; and the
phenomena of sunset and sunrise must therefore be very varied, and also
exquisitely beautiful, in worlds circling round such double suns. But
when each sun has a separate system, even more remarkable relations must
be presented. For each system of dependent worlds, besides its own
proper sun, must have another sun--less splendid, perhaps (because
farther off), but still brighter beyond comparison than our moon at the
full. And, according to the position of any planet of either system,
there will result for the time being either an interchange of suns,
instead of the change from night to day, or else double sunlight during
the day, and a corresponding intensified contrast between night and day.
Where the two suns are very unequal or very differently coloured, or
where the orbital path of each is very eccentric, so that they are
sometimes close together and at others far apart, the varieties in the
worlds circling round either, or around the common centre of both, must
be yet more remarkable. "It must be confessed," we may well say with Sir
John Herschel, "that we have here a strangely wide and novel field for
speculative excursions, and one which it is not easy to avoid
luxuriating in."'

Anyone who takes a cursory glance at the heavens on a clear night can
readily perceive that there exists considerable diversity of colour
among the stars. The contrast between some is pronounced and well
marked, whilst others exhibit refined gradations of hue.

The most numerous class of stars are those which are described as white
or colourless. They comprise about one-half of the stars visible to the
naked eye. Among the most conspicuous examples of this type are
Sirius--whose diamond blaze is sometimes mingled with an occasional
flash of blue and red--Altair, Spica, Castor, Regulus, Rigel, all the
stars of Ursa Major with the exception of one, and Vega--a glittering
gem of pale sapphire, almost colourless. The light emitted by stars of
this class gives a continuous spectrum, the predominating element being
hydrogen, having a very elevated temperature and under relatively high
pressure. The vapours of iron, sodium, magnesium, and other metals, are
indicated as existing in small quantities.

The second class of stars is that to which our Sun belongs. They are of
a yellow colour, and embrace two-thirds of the remaining stars. The most
prominent examples of this type are Arcturus, Capella, Aldebaran,
Procyon, and Pollux. Hydrogen does not predominate so much in these as
in the Sirian stars, and their spectra resemble closely the solar
spectrum, indicating that they are composed of elements similar to those
which exist in the Sun.

The star which bears the nearest resemblance to our Sun, both as regards
the colour of its light and physical structure, is Capella, the most
conspicuous star in the constellation Auriga, and one of the leading
brilliants in the Northern Hemisphere. Its spectrum presents all the
characteristics observed in the solar spectrum, and there exists an
almost identical similarity in their physical constitution, though
Capella is a much more magnificent orb than the Sun.

The third class of stars includes those which are of a ruddy hue, such
as Betelgeux in the right shoulder of Orion, Antares in Scorpio, and
Alpha Herculis. Their spectra present a banded or columnar appearance,
and there is greater absorption, especially of the blue rays of light.
It is believed that the temperature of stars of this colour is not so
elevated as that of those belonging to the other two orders, and that
this is a sufficient reason to account for the different appearance of
their spectra.

The aid of a good telescope is, however, necessary to enable us to
perceive the varied colours and tints of the sparkling gems with which
Nature has adorned her star-built edifice of the universe. Most of the
precious stones on Earth have their counterparts in the heavens,
presenting in a jewelled form contrasts of colour, pleasing harmonies,
and endless variety of shade. The diamond, sapphire, emerald, amethyst,
topaz, and ruby sparkle among crowds of stars of more sombre hue. Agate,
chalcedony, onyx, opal, beryl, lapis-lazuli, and aquamarine are
represented by the radiant sheen emanating from distant suns, displaying
an inexhaustible variety of colour, blended in tints of untold harmony.

It is among double stars that the richest and most varied colours
predominate. There are pairs of white, yellow, orange, and red stars;
yellow and blue, yellow and pale emerald, yellow and rose red, yellow
and fawn, green and gold, azure and crimson, golden and azure, orange
and emerald, orange and lilac, orange and purple, orange and green,
white and blue, white and lilac, lilac and dark purple, &c., &c. There
are companion stars revolving round their primaries, coloured olive,
lilac, russet, fawn, dun, buff, grey, and other shades indistinguishable
by any name.

Our knowledge of binary star systems brings us to what may be regarded
as the threshold of the fabric of the heavens. For it is known that
other systems exist into the construction of which numerous stars enter.
These form intricate and complex stellar arrangements, in which the
component stars are physically united and retained in their orbits by
their mutual attraction.




CHAPTER VII

THE STARRY HEAVENS


TRIPLE, QUADRUPLE, AND MULTIPLE STARS.--These, when observed with the
naked eye, appear as single stars, but, when examined with a high
magnifying power, each lucid point can be resolved into several
component stars. They vary in number from three to half a dozen or more,
and form systems of a more complex character than what are observed in
the case of binary stars. In the usual construction of a triple system,
the secondary star of a binary is resolvable into two, each star being
in mutual revolution, whilst they both gravitate round their primary. By
another arrangement, a close pair control the movements of a distant
attendant.

One of the most interesting of triple stars is the tricoloured Gamma
Andromedæ. The brilliant components of this system have their
counterparts in the topaz, the emerald, and the sapphire--the larger
star is of the third magnitude and of a golden yellow colour; the
secondary of the fifth magnitude and of an emerald green. These stars
are ten seconds apart, and, though they have been under observation
since 1777, no orbital movement has as yet been detected, but their
common proper motion indicates their close relationship and physical
connection. In 1842, Otto Struve discovered that the companion star is
itself double, and round it there gravitates a sapphire sun, which is
believed to accomplish a revolution of its orbit in about 500 years. If
round those suns there should be circling planetary systems of worlds
inhabited by intelligent beings, the varied effects produced by the
light emanating from those different coloured orbs would be of a very
beautiful and pleasing nature.

A system suggestive of the endless variety of stellar arrangement that
exists throughout the sidereal regions is apparent in the case of the
triple star Zeta Cancri. Two of the stars, of magnitudes six and seven,
form a binary in rapid revolution, the components of which complete a
circuit of their orbits in fifty-eight years, whilst the more distant
third star, of almost similar magnitude, accomplishes a wide orbital
ellipse round the other two in 500 or 600 years. These stars have been
closely observed by astronomers during the past forty years, with the
result that their motions have appeared most perplexing, and complicated
beyond precedent. 'If this be really a ternary system,' wrote Sir John
Herschel, 'connected by the mutual attraction of its parts, its
perturbations will present one of the most intricate problems in
physical astronomy.' The second star revolves round its primary, whilst
the third pursues a retrograde course, but its path, instead of being
even, presents the appearance of a series of circular loopings, in
traversing which the star alternately quickens and slackens its pace,
or at times appears to be stationary.

Astronomers have arrived at the conclusion that these perturbations are
produced by the presence of a fourth member, which, though invisible, is
probably the most massive of the system--perhaps a magnificent world
teeming with animated beings, and attended by three suns which gravitate
round it, dispensing light and heat to meet the requirements of the
various forms of life which exist on its surface. In this system we have
an arrangement the reverse of what exists in the solar system, where all
the planets revolve round a predominant sun; but here there is a strange
verification of the old Ptolemaic belief with regard to the path of a
sun, though in this instance there are three suns circling round a dark
globe which they illumine and vivify.

Triple stars occur with comparative frequency throughout the heavens. In
Monoceros there is a fine triple star, discovered by Herschel, which he
describes as 'one of the most beautiful sights in the heavens.' The
stars Xi and Beta Scorpii form triple systems in which the components
are differently arranged. In Xi the primary and secondary consist of two
revolving stars which control the movements of a distant attendant; in
Beta the primary and secondary stars are in mutual revolution, whilst
round the former there circles a very close minute companion. There are
doubtless many binary stars which, if examined with adequate telescopic
power, would resolve themselves into triple and multiple systems, but
the profound distances of those objects render the detection of their
components a most difficult task.

Quadruple stars are usually arranged in pairs, _i.e._ the primary and
secondary of a binary system are each resolvable into two, forming two
pairs, each pair being in mutual revolution, while they both gravitate
round their common centre of gravity. Epsilon Lyræ, which has been
described as a double double, is an example of a quadruple system, and
Nu Scorpii is of a similar construction, but more beautiful because its
components are in closer proximity to each other. Close upon twenty of
those double double systems have been discovered in different parts of
the heavens.

One of the most interesting of quadruple systems is Theta Orionis, which
is situated in the Great Nebula, by which it is surrounded. This star,
when observed with a telescope of low power, can be at once resolved
into four separate lucent points, so arranged as to form a quadrilateral
figure or trapezium. They are of the fifth, sixth, seventh, and eighth
magnitudes, and described as pale white, garnet, faint lilac, and red.
Though they have been under careful observation for upwards of two
centuries, no perceptible motion has been perceived as occurring among
them, nor has there been any change in their relative positions--they
appear to be perfectly motionless; but we must not infer from this that
no physical bond of union exists between them, for they are situated at
an amazing distance from the Earth. Ascending higher in the scale of
celestial architecture, we have multiple stars forming systems still
more elaborate and complex, into the structure of which numerous stars
enter, and they, as they increase in number, gradually merge into
star-clusters.

If we assume that around each of the components of a multiple star there
circles a retinue of planetary worlds, we are confronted with a most
perplexing problem as to how the dynamical stability of a system so
different from, and so vastly more complicated than, that of our solar
system is maintained--where, as it were, suns and planets
intermingle--how numerous circling orbs can accomplish their revolutions
without being swayed and deflected from their paths by the gravitational
attraction of adjacent members of the same system. Perplexing though the
arrangement of such a scheme may be to our conception, yet, each orb has
been weighed, poised, and adjusted by Infinite Wisdom, to perform its
intricate motions in synchronous harmony with other members of the
system--all moving in unison like the parts of a complicated piece of
mechanism, and maintained in stable equilibrium by their mutual
attraction--

    Mystical dance, which yonder starry sphere
    Of planets and of fixed in all her wheels
    Resembles nearest; mazes intricate,
    Eccentric, intervolved, yet regular
    Then most, when most irregular they seem;
    And in their motions harmony divine
    So smooths her charming tones that God's own ear
    Listens delighted.--v. 620-27.

All the natural phenomena with which we are familiar would, in the case
of planets revolving round the component suns of a multiple system, be
of a different kind or altogether absent. Instead of being illumined by
one sun, those worlds would, at certain times, have several suns--some
more distant than others--above their horizons, and upon very rare
occasions, if ever, would there be an entire absence of all of those
orbs from their skies. Consequently there would be no year such as we
are familiar with; no regular sequence of seasons similar to what is
experienced on Earth; no alternation of day and night, for there would
be '_no night there_,' though, in the absence of the primary orb, the
light emitted by distant suns, whilst sufficient to banish night, and
beyond comparison brighter than the Moon when at full, would, in the
diminution of its intensity from that of noonday, be as grateful a
change as that of from day to night which occurs on our globe.

Should those suns be differently coloured, each emitting its own
peculiar shade of light as it appears above the horizon, the varied
aspects of the perpetual day enjoyed by the inhabitants of those
circling worlds present to the imagination harmonies of light and shade
over which it is pleasant to linger.

TEMPORARY, PERIODICAL, AND VARIABLE STARS.--It may seem remarkable that
among so many thousands of stars which spangle the firmament, there
should occur no very perceptible change or variation in their aspect
and brilliancy. From age to age they present the same appearance, shine
with the same undiminished splendour, and rise and set with the same
regularity. So that from time immemorial the stars have been regarded by
mankind as the embodiment of all that is eternal and unchangeable. Yet,
the serenity of the celestial regions does not always remain
undisturbed--at occasional times a 'Nova,' or new star, blazes forth
unexpectedly in the heavens, and perplexes astronomers; and, after
shining with a varying degree of brilliancy for a few weeks or months,
gradually diminishes in size and brightness and eventually becomes lost
to sight.

A record has been kept of about twenty temporary stars that have been
observed at various periods since the time that reliable data of those
objects have been published. Pliny mentions the appearance of a new star
in the time of Hipparchus (134 B.C.); it was seen in the constellation
of the Scorpion, and it is said that it was the apparition of this star
which induced the celebrated astronomer to construct what is known as
the earliest star catalogue. A new star is said to have become visible
when the Emperor Honorius ruled, and another during the reign of the
Emperor Otho, about 945 A.D. In May 1012 a new star appeared in Aries,
and in July 1203 another was observed in Scorpio, which resembled
Saturn. The most remarkable star of this kind was one observed by Tycho
Brahé, which appeared in the constellation Cassiopeia. He first
perceived it on November 11, 1572. In lustre it equalled Jupiter, and
when at its brightest rivalled Venus; it was visible at noonday, and at
night its light could be perceived through strata of cloud which
rendered all other stars invisible. The star maintained its brilliancy
for three weeks, when it became of a yellowish colour and perceptibly
decreased in size; it afterwards assumed a ruddy hue resembling
Aldebaran, and, diminishing gradually in magnitude and brightness,
ceased to be visible in March 1574. It twinkled more than the other
stars, and during the time it could be perceived its position remained
unchanged. In 1604 a conspicuous new star burst forth in Ophiuchus. It
surpassed in brilliancy stars of the first magnitude, and outshone the
planet Jupiter, which was in its proximity. Kepler observed this star,
and described it as 'sparkling like a diamond with prismatic tints.' It
soon began to decline after its appearance; in March 1605 it had shrunk
to the dimensions of a third-magnitude star, and in a year later it
became entirely lost to view. Other stars of the same class, though of a
less conspicuous character, have been observed at occasional times.
Anthelme, a Carthusian monk, discovered one near Beta Cygni in 1670;
another appeared in Ophiuchus in 1848; one in Scorpio in 1860; one in
Corona Borealis in 1866; in Cygnus in 1876; in Andromeda in 1885; and in
Auriga in 1892.

Various theories have been advanced in order to account for the sudden
outbursts of those stars, the light from which has probably occupied
not much less than one hundred years in its passage hither. It has been
suggested that the collision of two suns, or of two great masses of
matter, would create such phenomena; but, apart from the improbability
of such a catastrophe occurring among the celestial orbs, the rapid
subsidence in the luminosity of the observed objects would indicate that
the outburst was produced by causes of a more rapidly transitory nature
than what would result from the collision of two condensed masses of
matter. A collision occurring between two swarms of meteors has been
suggested as one way of accounting for the sudden appearance of those
stars; but another, and more plausible, explanation is that they are
produced by a great eruption of glowing gas from the interior of a sun,
causing an enormous increase in its luminosity, which subsides after a
time, and is succeeded by a normal condition of things. It has been
observed that all those temporary stars, with the exception of two, have
appeared in the region of the Milky Way. In this luminous zone the
condensation of small gaseous stars and nebulæ is more pronounced than
in any other part of the heavens, and this would seem to indicate that
there may be cosmical changes taking place among them which need not be
associated with the occurrence of catastrophes resulting in the
conflagration of worlds, and that Nature, in accomplishing her purposes,
does not overstep the uniform working of her laws, upon which depend the
stability and existence of the universe.

PERIODICAL AND VARIABLE STARS are distinguished from other similar
objects by the fluctuations which occur in the quantity of light emitted
by them. The difference in the luminosity of some stars is at times so
marked that, in a few weeks or months, they decline from the first or
second magnitudes to invisibility, and, after the expiration of a
certain period, they again gradually regain their pristine condition.
When these changes take place with regular recurrence, they are called
'periodical;' when they occur in a variable and uncertain manner, they
are called 'irregular.' About 300 stars are known as variable, but the
majority of them are telescopic objects. Their periodical changes of
brilliancy present every degree of variety; in some stars they are
scarcely perceptible and occur at long intervals; in others, changes of
brightness occur in a few hours or days, by which the light emitted is
intensified many hundreds of times.

Some stars accomplish their cycle of change in a few days, many in a few
weeks or months, and there are others which do not complete their
periods until the expiration of a number of years.

One of the most remarkable of variable stars is called Mira 'the
wonderful,' in the constellation Cetus. When at its maximum brilliancy
it shines for two or three weeks as a star of the second magnitude. It
then begins to gradually decline, and at the end of three months becomes
invisible. It remains invisible for five months, and then reappears, and
during the ensuing three months it regains by degrees its former
brilliancy. Mira completes a cycle of its changes in 334 days, and,
during that time, oscillates between a star of the second and tenth
magnitude. The variability of Mira Ceti was first observed by David
Fabricius in the sixteenth century.

Another remarkable star is Eta Argus, which is surrounded by the great
nebula in the constellation Argo Navis. It is invisible to the naked
eye, but in the telescope it has a reddish appearance, and is slightly
brighter than the stars in its vicinity. It was first observed by Halley
in 1677, and it was then of the fourth magnitude. In 1751 it had risen
to the second magnitude, and maintained its position as a star of this
class until 1837, when, on December 16 of that year, its brilliancy
suddenly increased, and it equalled in a short time Alpha Centauri. It
reached its maximum in 1843, and then it was surpassed only by Sirius.
It maintained its brilliancy for about ten years. In 1858, it declined
to the second magnitude, in 1859 to the third, and, gradually
diminishing, it became invisible to the naked eye in 1868. It is now of
the seventh magnitude, and is again increasing, and may soon resume its
position among the other stars. It is believed to have a period of
seventy years, and in that time its light ebbs and flows between the
seventh and first magnitudes.

The most interesting variable star in the heavens is Algol (the demon),
in the constellation Perseus. Its light fluctuations can be observed
without the aid of a telescope, and it completes a cycle of its changes
in two or three days. For about two days and thirteen hours it is
conspicuously visible as a star of the second magnitude; it then begins
to decline, and in about four hours sinks to the dimensions of a
fourth-magnitude star; it remains in this condition for twenty minutes,
and then increases gradually until, at the expiration of four hours, it
regains its former brilliancy, which it sustains for two days and
thirteen hours, when it again goes through the same cycle of changes in
a precisely similar manner to what has been described. Astrologers have
ascribed many evil influences to the demon star, which adorned the head
of Medusa; nor did it escape the observation of ancient astronomers that
this malevolent orb is--as a modern writer amusingly remarks--slowly
winking at us from out the depths of space.

Variable stars are found in greater numbers in some parts of the heavens
than in others. Those of a white colour, and with shorter and more
regular periods, are most numerous in the region of the Milky Way; those
that are small, with long periods and of a reddish hue, are more widely
removed from that zone. Stars of this class are all very remote, and no
attempt has as yet been made to ascertain the parallax of Algol.

Several theories have been suggested in order to account for the
periodical brilliancy of those stars. It has been suggested that the
stars have opaque non-luminous patches on their surfaces, and that
during axial rotation their light ebbs and flows according as the dark
or bright portions are turned towards us. This theory is highly
improbable. Another and more plausible reason, especially with regard to
short period variables, is, that around those stars there revolve opaque
bodies or satellites which at times intercept a portion of their light
by producing a partial eclipse of their discs, similar to that caused by
the dark body of the Moon when passing between the Sun and the Earth.

It is now known that in the case of variables of the Algol type, the
periodical fluctuations of their light arises from this cause, and that
round Algol there is a dark world or satellite travelling, which
completes a revolution of its orbit in about sixty-nine hours, and that,
during each circuit, it intercepts one half of the light of its primary
by partially eclipsing the orb, and thereby creating a diminution in its
apparent magnitude which becomes perceptible at recurring intervals.

STAR GROUPS.--These are plentifully scattered over the heavens and, by
their conspicuous brilliancy, add to the grandeur and magnificence of
the midnight sky. The Hyades in Taurus, of which Aldebaran is the chief,
forming the eye of the Bull, attract attention.

The stars in Coma Bernices form a rich group; the sickle in Leo, the
seven stars in Ursa Major, and those in Cassiopeia and Aquila are
familiarly known to all observers. Besides these, there are many other
groups and aggregations of stars which adorn the celestial vault and
enhance the beauty of the heavens.

STAR CLUSTERS.--On observing the heavens on a clear, dark night, there
can be seen in different parts of the sky closely aggregated groups of
stars called clusters. In some instances the component stars are so near
together that the naked eye is unable to discern the individual members
of the cluster. They then assume an indistinct, hazy, cloudlike
appearance. Upwards of 500 clusters are known to astronomers, the
majority of which are very remote. Many of them contain thousands of
stars compressed into a very small space, and others are so distant that
the largest telescopes are incapable of resolving their nebulous
appearance into separate stars.

Star clusters have been arranged into two classes, 'irregular' and
'globular;' but no sharp line of demarcation exists between them, though
each have their distinctive peculiarities. Irregular clusters consist of
aggregations of stars brought promiscuously together, and presenting an
appearance devoid of any structural arrangement. They are of different
shapes and sizes, possess no distinct outline, and are not condensed
towards their centre, like those that are globular. On examination, they
present an intricate reticulated appearance; streams and branches of
stars extend outwards from the parent cluster, sometimes in rows and
sinuous lines, and, in other instances, diverging from a common centre,
forming sprays. Sometimes the stars are seen to follow each other on the
same curve which terminates in loops and arches of symmetrical
proportions.

There are three conspicuous clusters in the northern sky that are
visible to the naked eye--viz. the Pleiades in Taurus, the Great Cluster
in the sword-handle of Perseus, and Praesepe in Cancer, commonly called
the Beehive.

The cluster which from time immemorial has had bestowed upon it the
chief attention of mankind are the beautiful Pleiades or Seven Sisters,
and intertwined among its stars are the legendary and mythological
beliefs of ancient nations and untutored tribes inhabiting the different
regions of the globe. When viewed with a telescope of moderate size the
cluster appears as a scattered group, and numerous stars become visible
that are imperceptible to ordinary vision.

In the sword-handle of Perseus there is a cluster which, to the naked
eye, appears as a small patch of luminous cloud. This inconspicuous
object when observed with an instrument of moderate power is resolved
into a magnificent assemblage of stars, and presents a spectacle which
creates in the mind of the beholder mingled feelings of admiration and
amazement. No telescope has yet penetrated its utmost depths, or
revealed all the glories of this shining region, crowded with glittering
points of light comparable in number to the pebbles strewn on the shore
of a troubled sea.

The cluster Praesepe in Cancer is visible on a clear night to the
unaided eye as a small nebula. This object attracted the attention of
Galileo, to which he applied his newly invented telescope, and was
delighted to find that his glass was capable of resolving it into a
group of stars thirty-six in number, and all of comparatively large
magnitude. The disappearance of Praesepe in consequence of the
condensation of vapour in the atmosphere was regarded by the ancients as
a sure indication of approaching rain. In the same constellation, near
the Crab's southern claw, there is another rich cluster, which consists
of 200 stars of the ninth and tenth magnitudes.

In Sobieski's Shield there is a magnificent fan-shaped cluster of minute
stars with a prominent one in its centre; and in the constellation of
the Southern Cross there is a cluster which, on account of the varied
colours of its component stars, has been compared by Sir John Herschel
to 'a piece of rich fancy jewellery;' eight of the principal stars being
coloured red, green, and blue.

GLOBULAR CLUSTERS.--These have been described by Herschel as 'the most
magnificent objects that can be seen in the heavens.' They are all very
remote, of a rounded form, and when viewed with a telescope present the
appearance of 'a ball of stars.' In some clusters the constituent stars
are distinguishable as minute points of light; in others, more remote,
they are of a coarse granular texture, and in those still more distant
they resemble a 'heap of golden sand.' Some clusters are situated at
such a profound distance in space that it is impossible with the most
powerful of telescopes to define their stellar structure; all that can
be distinguished of these is a cloudy luminosity resembling in
appearance an irresolvable nebula. Globular clusters usually present a
radiated appearance. Rays, branches, and spiral-shaped streams of stars
appear to flow from the circumference of some; and, in other instances,
fantastic appendages of stars project outwards from the parent cluster.
There doubtless exists much variety in the structural arrangement of
these clusters, and an equal diversity in the magnitude and number of
the stars which enter into their formation. The stars in some clusters
may equal those of the first magnitude, and in others they may not
exceed in dimensions the minor planets. In the telescope they vary in
size from the eleventh to the fifteenth magnitude; the smaller stars
occupy the centre of a cluster, whilst the larger ones are found near
its circumference. Globular clusters are more condensed towards their
centre than those of irregular shape, and some have a nucleated
appearance. This apparent condensation is not altogether owing to the
depth of star strata as viewed from the circumference of the cluster,
but there appears to exist an attractive force (probably gravitational)
which draws the stars towards its centre, and if this 'clustering power'
were not opposed by some other counteracting force, those bodies would
coalesce into one mass. It may be 'that a centrifugal impulse
predominates by which full-grown orbs are driven from the nursery of
suns in which they were reared to seek their separate fortunes and enter
on an independent career elsewhere.'

It is not known how the dynamical equilibrium of a star cluster is
maintained; and on account of its extreme distance no motion is
perceptible among its component stars. The laws by which those stellar
aggregations are produced and governed are wrapped in obscurity, and the
nature of the motions of their stars, whether towards concentration or
diffusion, cannot at present be ascertained. If those globular clusters
could be observed sufficiently near, they would most probably expand
into vast systems of suns occupying immense regions of space.

The largest and most magnificent globular cluster in the heavens is
Omega Centauri, in the Southern Hemisphere. To the naked eye it
resembles a round, indistinct, cometary object, about equal to a star of
the fourth magnitude; but when observed with a powerful telescope it
appears as a globe of considerable dimensions composed of innumerable
stars of the thirteenth and fifteenth magnitudes, all exceedingly minute
and gathered into small knots and groups. A remarkable cluster in
Toucani is described by Sir John Herschel as 'most magnificent; very
large; very bright, and very much compressed in the middle.' The
interior mass consists of closely aggregated pale rose-coloured stars,
surrounded by others of a pure white which embrace the remainder of the
cluster. There is a fine globular cluster in Sagittarius between the
Archer's head and the bow. It was observed by Hevelius in 1665. The
central portion is very much compressed, and consists of excessively
minute stars enclosed by others of larger size. In Aquarius there is a
magnificent ball of stars of a beautiful spherical form, which Sir J.
Herschel compared to a heap of fine sand. Numerous other clusters are
profusely distributed over the heavens, occupying regions in the
profound depths of space which can only be reached by the aid of most
powerful instruments.

The finest and most remarkable object of this class visible in the
northern heavens is the Great Cluster which lies between Eta and Zeta
Herculis. It was discovered by Halley in 1714, who writes: 'This is but
a little patch, but it shows itself to the naked eye when the sky is
serene and the moon absent.' When observed with a powerful telescope its
magnificence at once becomes apparent to the beholder. 'Perhaps,' says
Dr. Nichol, 'no one ever saw it for the first time through a telescope
without uttering a shout of wonder.' At its circumference the stars are
rather scattered, but towards the centre they appear so closely
aggregated that their combined effulgence forms a perfect blaze of
light. Sir William Herschel estimated that there are 14,000 stars in the
cluster, each a magnificent world but unaccompanied by any planetary
attendants.

[Illustration: CLUSTER IN HERCULES]

As a result of more recent investigations this number has been
considerably reduced, and it is now generally believed that about 4,000
stars enter into the formation of the cluster. As its distance from the
Earth is unknown, it follows that there must be some uncertainty
attached to any conclusions that may be arrived at with regard to this
superb object. Miss Agnes Clerke estimates the number of the constituent
stars at 4,000, and in support of her conclusion this talented lady
writes as follows: 'The apparent diameter of this object, including most
of the "scattered stars in streaky masses and lines" which form a sort
of "glory" round it, is 8´; that of its truly spherical portion may be
put at 5´. Now, a globe subtending an angle of 5´ must have (because the
sine of that angle is to radius nearly as to 1 : 687) a real diameter
1/687 of its distance from the eye, which, if we assume to be such as
would correspond to a parallax of 1/20 of a second, we find that the
cluster, outliers apart, measures 558,000 millions of miles across.
Light, in other words, occupies thirty-six days in traversing it, but
sixty-five years in journeying thence hither. Its components may be
regarded, on an average, as of the twelfth magnitude; for, although the
divergent stars rank much higher in the scale of brightness, the central
ones, there is reason to believe, are notably fainter. The sum total of
their light, if concentrated into one stellar point, would at any rate
very little (if at all) exceed that of a third-magnitude star. And one
star of the third is equivalent to just four thousand stars of the
twelfth magnitude. Hence we arrive at the conclusion that the stars in
the Hercules Cluster number much more nearly four than fourteen
thousand.'

For what purpose do those thousands of clustering orbs shine? Who can
tell? Night is unknown in the regions illumined by their brilliant
radiance. This stupendous aggregation of suns testifies to the
magnificence of the starry heavens, and to the omnipotence of the
Creator.

GALAXIES.--These consist of vast aggregations of stars which form
separate 'island universes' floating in the depths of space; they are
believed to equal in magnitude and magnificence the Milky Way--the
galaxy to which our system belongs.

NEBULÆ.--We now reach the last, and what are believed to be the most
distant of the known contents of the heavens. They are all exceedingly
remote, devoid of any perceptible motion, faintly luminous, and, with
the exception of two of their number, invisible to the naked eye. Halley
was the first astronomer who paid any attention to those objects. In
1716 he enumerated six of them, but of this number only two can, in a
strict sense, be regarded as nebulæ, the others since then have been
resolved into magnificent star clusters. In 1784, Messier catalogued 103
nebulæ, and the Herschels--father and son--in their survey of the
stellar regions, discovered 4,000 of those objects. There are now 8,000
known nebulæ in the heavens, but the majority of them are not of much
interest to astronomers. Prior to the invention of the spectroscope it
was believed that all nebulæ were irresolvable star clusters, but the
analysis of their light by this instrument indicated that their
composition was not stellar but gaseous. Their spectra consist of a few
bright lines revealing the presence of hydrogen, nitrogen, and other
gaseous elements.

Much that is mysterious and uncertain is associated with those objects
which appear to lie far beyond the limits of our sidereal system. It is
now generally believed that they exhibit the earliest stage in the
formation of stars and planets--inchoate worlds in process of slow
evolution, which will eventually condense into systems of suns, and
planetary worlds.

Nebulæ present every variety of form. Some are annular, elliptic,
circular, and spiral; others are fan-shaped, cylindrical, and irregular,
with tufted appendages, rays, and filaments. A fancied resemblance to
different animated creatures has been observed in some. In Taurus there
is a nebula called the 'Crab' on account of its likeness to the
crustacean; another is called the 'Owl Nebula' from its resemblance to
the face of that bird. The Orion Nebula suggests the opened jaws of a
fish or sea monster, hence called the Fish-Mouth Nebula. There is a
Horse-Shoe Nebula, a Dumb-Bell Nebula, and many others of various shapes
and forms. They are classified as follows: (1) Annular Nebulæ, (2)
Elliptic Nebulæ, (3) Spiral Nebulæ, (4) Planetary Nebulæ, (5) Nebulous
Stars, (6) Large Irregular Nebulæ.

ANNULAR NEBULÆ.--These resemble in appearance an oval-shaped luminous
ring; they are comparatively few in number, and not more than a dozen
have been discovered in the whole heavens. The most remarkable object of
this class is the Ring Nebula, which is situated between the stars Beta
and Gamma Lyræ. It is visible in a moderate-sized telescope as a
well-defined, flat, oval ring; its central part is not quite dark but is
occupied by a filmy haze of luminous matter which is prolonged inwards
from the margin of the ring. When examined with a high power the edges
of the ring have a fringed appearance, and numerous glittering stellar
points become visible both within and without its circumference. This
nebulous ring, though a small object in the telescope, is of enormous
magnitude, and if it were not more distant than 61 Cygni, one of the
nearest of the fixed stars, its diameter would not be less than 20,000
millions of miles, but it has been estimated by Herschel that it is 900
times more remote than Sirius. How stupendous, then, must be its
dimensions, and how bewildering to our conception is the profound
immensity of space in which it is located! An annular nebula similar to
that of Lyra, but on a smaller scale, is found in Cygnus, and within it
there can be seen a conspicuous star. Another exists in Scorpio which
contains two stars situated within the ring at diametrically opposite
points to each other.

ELLIPTICAL NEBULÆ.--The most interesting object of this class is the
Great Nebula in Andromeda, called 'the transcendentally beautiful queen
of the nebulæ'--an appellation which it scarcely merits. This object,
which is plainly visible to the naked eye, is of an oval shape, of a
milky white colour, and is situated near the most northern star of the
three which form the girdle of Andromeda. It was known to the ancients,
and Ali Sufi, a Persian astronomer who flourished in the tenth century,
alludes to it; but it did not attract much attention until the
seventeenth century. Simon Marius was the first to observe this object
with a telescope. This he did on December 15, 1612; he describes it as
shining with a pale white light resembling in appearance the flame of a
candle when seen through a semi-transparent piece of horn. When examined
with a high magnifying power it is seen to occupy a largely extended
area measuring 4° in length and 2-1/2° in breadth. Its luminosity
increases from the circumference to the centre, where there can be seen
a small nucleus with an ill-defined boundary, which has the appearance
of being granular, but its composition is not stellar. Two dark channels
running almost parallel to each other and to the axis of the nebula have
been observed by Bond; these, when prolonged, form into curves which
terminate in two great rings. They are wide rifts which separate streams
of nebulous matter, and are indicative that some formative processes may
be going on within the nebula.

Astronomers have been baffled in their attempts to discover the nature
of the Andromeda Nebula. Though great telescopes have been able to
render visible thousands of stars over and around it, yet the nebula
itself is irresolvable and bears no trace of stellar formation;
neither, according to Dr. Huggins, is its spectrum gaseous, a
circumstance which deepens the mystery associated with this object. Its
distance is unknown, and its dimensions cannot be ascertained.

Other elliptical nebulæ are found in different regions of the heavens.
In Ursa Major there is an oval nebula resembling that of Andromeda, but
on a much smaller scale. It possesses a nucleus, and on the photographic
plate there can be detected the presence of spiral structure, indicating
the existence of streams of nebulous matter. Adjacent to this nebula is
another of the same class with a double nucleus, and associated with it
is a nebulous star.

SPIRAL NEBULÆ.--The great reflector of Earl Rosse at Parsonstown was the
successful means by which nebulæ of this form were discovered. This
powerful telescope was capable of defining with greater accuracy the
structural formation of those objects than any other instrument in use.
It was ascertained that spiral coils and convoluted whorls enter into
the structure of most nebulæ, indicating a similarity in the process of
change which may be going on in these vast accumulations of cosmical
matter. The most interesting specimen of a spiral nebula is situated in
Canes Venatici. It consists of spiral coils emanating from a centre with
a nucleus and surrounded by a narrow luminous ring. In appearance it
resembles the coiled mainspring of a watch.

PLANETARY NEBULÆ.--These have been so named on account of the
resemblance which they bear to the discs of planets. They are of uniform
brightness, circular in shape, with sharply-defined edges, and are
frequently of a bluish colour. They are more numerous than annular
nebulæ; three-fourths of their number are in the Southern Hemisphere,
and they are situated in or very near the Milky Way. Those objects were
first described by Sir William Herschel, who was rather perplexed as to
what was their real nature and how he should classify them. He remarked
that they could not be planets belonging to far-off suns, nor distant
comets, nor distended stars. Consequently, he concluded rightly that
they were nebulæ. When observed with large telescopes, they lose their
planetary aspect, and their sharpness of outline is less apparent; their
discs become broken up into bright and dark portions, and in some,
numerous minute stars have been observed, whilst others have
well-defined nuclei.

The most prominent nebula of this class is situated in the constellation
Ursa Major, and is called the Owl Nebula, from its fancied resemblance
to the face of that bird. Sir John Herschel describes it as 'a most
extraordinary object, a large, uniform nebulous disc, quite round, very
bright, not sharply defined, but yet very suddenly fading away to
darkness.' When examined in 1848 with Earl Rosse's reflector, two bright
stars were discovered in its interior; each was in the centre of a
circular dark space surrounded by whorls of nebulous matter--hence the
origin of its name. This nebula gives a bright line spectrum indicative
of gaseous composition. It is believed to consist chiefly of hydrogen
and other gases which form a globe of such stupendous magnitude that, if
we surmise its distance from the earth to be sixty-five light years--an
estimate much too low--'its diameter would exceed that of the orbit of
Neptune upwards of 100 times.'[10] Within its compass the orbs of
hundreds of solar systems as large as that of ours would be able to
perform their revolutions, having spacious intervals existing between
each system. Another interesting planetary nebula is in the
constellation of the Dragon, near to the pole of the ecliptic; it is
slightly oval, of a pale blue colour, and contains a star of the
eleventh magnitude in its centre. It gives a gaseous spectrum. Attempts
have been made to determine its parallax, but without success, and
during the eighty years it has been under observation it has remained
apparently motionless. Its light period, if estimated at 140 years,
would indicate the existence of a globe with a diameter equal to
forty-four diameters of the orbit of the planet Neptune.[11] A nebula of
this class was discovered by Sir John Herschel in the Centaur. He
described it as resembling Uranus, but larger; its colour was of a
beautiful rich blue, and its light equalled that of a star of the
seventh magnitude.

NEBULOUS STARS.--These stars are each surrounded by a luminous haze
several minutes of arc in diameter and of a circular form. Sir William
Herschel, by his observation of those objects, arrived at the conclusion
'that there exists in space a shining fluid of a nature totally unknown
to us, and that the nebulosity about those stars was not of a starry
nature.' Thirteen stars of this type have been enumerated by him and
many others have since been discovered. The 'glow' which surrounds them
has been observed in a few instances to have vanished without leaving
any trace of nebulosity behind, but the causes which have brought about
such a result are entirely unknown. The nature of those stars is
involved in considerable obscurity, and one class of nebula would seem
to merge into the other; nebulous stars with faint aureolæ do not differ
much from small nebulæ interspersed with stellar points.

LARGE IRREGULAR NEBULÆ.--These are found in both hemispheres, and are
remarkable on account of the varied appearances which they present, and
the large extent of space which many of them occupy. In some, the
nebulous matter of which they are composed can be seen like masses of
tufted flocculi, sometimes piled up, and at other times promiscuously
scattered, resembling in appearance the foam on the crested billows of a
surging ocean rendered suddenly motionless, or cirro-cumuli floating in
a tranquil sky. Islands of light with intervening dark channels,
promontories projecting into gulfs of deep shade, sprays of luminous
matter, convoluted filaments, whorls, wreaths, and spiral streams all
enter into the structural formation of a great nebula.

The Great Nebula in Argo, in the Southern Hemisphere, is one of the most
remarkable objects of this class. It consists of bright irregular masses
of luminous matter, streaks and branches, and occupies an area about
equal to one square degree. At its eastern border is situated the
variable star Eta Argus, which fluctuates between the first and seventh
magnitudes in a period of about seventy years.

A rich portion of the Galaxy lies in front of the nebula, which creates
an effect as if it were studded over with stars. Sir John Herschel, in
describing this nebula, writes as follows:--'The whole is situated in a
very rich and brilliant part of the Milky Way, so thickly strewed with
stars that, in the area occupied by the nebula, not less than 1,200 have
been actually counted. Yet it is obvious that these have no connection
whatever with the nebula, being, in fact, only a simple continuation
over it of the general ground of the Galaxy. The conclusion can hardly
be avoided that, in looking at it, we see through and beyond the Milky
Way, far out into space, through a starless region, disconnecting it
altogether from our system. It is not easy for language to convey a full
impression of the beauty and sublimity of the spectacle which this
nebula offers as it enters the field of view of a telescope, fixed in
right ascension, by the diurnal motion, ushered in as it is by so
glorious and innumerable a procession of stars, to which it forms a sort
of climax, and in a part of the heavens otherwise full of interest.'
Another large bright nebula (called 30 Doradus), also in the Southern
Hemisphere, is composed of a series of loops with intricate windings
forming a kind of open network against the background of the sky which
it adorns. Sir John Herschel describes it as one of the most
extraordinary objects in the heavens.

The 'Crab' Nebula in Taurus, the 'Horse-Shoe' Nebula in Sobieski's
Shield, and the 'Dumb-Bell' Nebula in Vulpecula are remarkable objects,
but the assistance of a powerful telescope is required to bring out
their distinctive features. The 'Crab' Nebula is partially resolvable
into stars; the other two are believed to be gaseous.

The largest and most remarkable of all the nebulæ is that known as the
Great Nebula in Orion, which was discovered and delineated by Huygens in
the middle of the seventeenth century. It is perceptible to the naked
eye, and when viewed with a glass of low power can be seen as a circular
luminous haze surrounding the multiple star Theta Orionis--one of the
stars in the Giant's Sword, and which is of itself a remarkable object.
The most conspicuous part of the nebula bears a slight resemblance to
the wing of a bird; it consists of flocculent masses of nebulous matter
possessing a faint greenish tinge. Sir John Herschel compared it to a
surface studded over with flocks of wool, or to the breaking up of a
mackerel sky when the clouds of which it consists begin to assume a
cirrous appearance. Its brightest portion is occupied by four
conspicuous stars, which form a trapezium; around each there is a dark
space free from nebulosity, a circumstance which would seem to indicate
that the stars possess the power either of absorbing or of repelling the
nebulous matter in their immediate vicinity. When observed with a
powerful telescope, this nebula appears to be of vast dimensions, and,
with its effluents, occupies an area of 4° by 5-1/2°. Irregular
branching masses, streams, sprays, filaments, and curved spiral wreaths
project outward from the parent mass, and become gradually lost in the
surrounding space. This object remained for long a profound mystery; no
telescope was capable of resolving it, nor was it known what this
'unformed fiery mist, the chaotic material of future suns,' was, until
the spectroscope revealed that it consists of a stupendous mass of
incandescent gases--nitrogen, hydrogen, and other elementary substances,
occupying a region of space believed by some to equal in extent the
whole stellar system to which our Sun belongs.

In the Southern Hemisphere, near to the pole of the equator, are two
nebulous clouds of unequal size; the larger having an area about four
times that of the smaller. They are known as the Magellanic Clouds,
having been called after the navigator Magellan. Both are visible on a
moonless night, but in bright moonlight the smaller disappears. Sir John
Herschel, when at the Cape of Good Hope, examined those objects with his
powerful telescope. He described them 'as consisting of swarms of stars,
globular clusters, and nebulæ of various kinds, some portions of them
being quite irresolvable, and presenting the same milky appearance in
the telescope that the nebulæ themselves do to the naked eye.' These are
believed to be other universes of stars sunk in the profound depths of
space, our knowledge of their existence being dependent upon the faint
nebulous light which left them, perhaps, several thousand years ago.

[Illustration: GREAT NEBULA IN ORION]

The description of the various kinds of nebulæ leads us to consider what
is called the Nebular Hypothesis. That the stars and solar system had at
some time in the past a beginning, is as much a matter of certainty as
that they will at some future time cease to be. Stars, like organic
beings, have their birth, grow and arrive at maturity, then decline into
a state of decrepitude, and finally die out. The duration of the life of
a star, which may be reckoned by millions of years, depends upon the
length of time during which it can maintain a temperature that renders
it capable of emitting light. By the constant radiation of its heat into
space, a condition of its constituent particles consequent upon the
gradual contraction of its mass will ultimately occur, which will result
in the exhaustion of its stores of thermal energy, the extinction of its
light, and the reduction of what was once a brilliant orb to the
condition of a mass of cold, opaque, inert matter. Inquiries as to the
origin of the stars have led scientific men to conclude that they have
been evolved from gaseous nebulæ, and these have therefore been regarded
as indicating the earliest stage in the formation of suns and planets.
It is believed that the condensation of those attenuated masses of
luminous matter into stars is capable of accounting for the generation
and formation of all the shining orbs which enter into the structure of
the starry heavens. In the evolution of a 'cosmos out of a chaos' we
should expect to find stars presenting every stage of development--some
in an embryo state and others more advanced; stars in full vigour and
activity, stars that have passed the meridian of life, and stars in a
condition of decay and on the verge of extinction. The observations of
astronomers have led them to conclude that this condition of 'youth and
age' exists among the stellar multitude; but the characteristics by
which it is distinguished are neither very obvious nor reliable.

The nebular theory is incapable of proof or demonstration; but modern
discoveries tend to support the accuracy of its conclusions, and its
principles have now been adopted by the majority of philosophic
thinkers. The physical changes which are going on in the nebulæ towards
stellar evolution, or in fully formed stars towards dissolution, are so
slow that the life of an individual, or even the historical records of
the past, are incapable of furnishing any evidence of alteration in
their condition. A period of time infinitely greater than what has
elapsed since the birth of science must pass before anything can be
known of the life history of the stars; indeed, the allotted span of
man's existence on this planet may have terminated ere the evolution of
a large nebula into a star cluster can have taken place.

The nebular hypothesis was first propounded by Kant, who suggested that
the sun and planets originated from a vast and diffused mass of cosmical
matter. This theory was afterwards supported by Herschel and by the
great French astronomer Laplace. As a result of close and continued
observation of the different classes of nebulæ, Herschel arrived at the
conclusion that there exists in space a widely diffused 'shining fluid,'
of a nature totally unknown to us, and that the nebulosity which he
perceived to surround some stars was not of a starry nature. He further
adds that this self-luminous matter 'seemed more fit to produce a star
by its condensation than to depend on the star for its existence.' His
sagacious conclusion with regard to the non-stellar nature of this
nebulous matter was afterwards confirmed by the spectroscope; for at
that time it was believed that even the faintest nebulæ were
irresolvable star clusters.

In 1811 Herschel read a paper before the Royal Society in which he
propounded his famous nebular hypothesis, and stated his reasons for
believing that nebulæ, by their gradual condensation, were transformed
into stars. Having assumed that there exists a highly attenuated
self-luminous substance diffused over vast regions of space, he
endeavoured to show that by the law of attraction its particles would
have a tendency to coalesce and form aggregations of nebulous matter,
and that each of these, by the continued action of the same force, would
gradually condense and ultimately acquire the consistence of a star. In
the case of large irregular nebulæ, numerous centres of attraction would
originate in the mass, round which the nebulous particles of matter
would arrange themselves; each nucleus, when condensation had been
completed, would become a star, and the entire nebula would in this
manner be transformed into a cluster of stars. Herschel believed that he
could trace the different stages of nebular condensation which result in
the evolution of a star. In large, faintly luminous nebulæ the process
of condensation had only commenced; in others that were smaller and
brighter it was in a more advanced stage; in those that contained nuclei
there was evidence of nascent stars; and, finally, there could be seen
in some nebulæ minute stellar points--new-born suns--interspersed among
the haze of the transforming mass. By this theory Herschel was able to
account for the phenomena associated with nebulous stars and the
supposed changes which were observed in some nebulæ. The nebular
hypothesis as described by Herschel was not received with much favour,
nor did it unsettle much the belief that all nebulæ were vast stellar
aggregations, and that their cloudy luminosity was a consequence of the
inadequacy of telescopic power to resolve them into their component
stars. Laplace, who was highly gifted as a geometrician, demonstrated
how the solar system could have been evolved in accordance with
dynamical principles from a slowly rotating and slowly contracting
spheroidal nebula. The rotatory motion of a nebula, in obedience to a
well-known mechanical law, increases as its density becomes greater, and
this goes on until the tangential force at the equator overcomes the
gravitational attraction at its centre. When this occurs, a revolving
ring of nebulous matter is thrown off from the parent mass, and by this
means equilibrium is restored between the two forces. As the rotatory
velocity of the nebula continues to increase with its contraction,
another ring is cast off, and in this manner a succession of revolving
rings may be detached from the condensing spheroid; each newly-formed
ring being nearer to the centre of the contracting mass and revolving in
a shorter period than its predecessor. In the evolution of our system,
the central mass of the nebula became the Sun and each of the revolving
rings, by their condensation into one mass, formed a planet. In a
similar manner, though on a diminished scale, the elementary planets,
whilst in a nebulous state, parted with annular portions of their
substance, out of which were evolved their systems of satellites. This
theory furnished a plausible reason, which was capable of explaining how
the orbs which constitute the solar system came into existence, and,
though hypothetical, yet the manner in which it accounted for the
orderly and symmetrical genesis of the system rendered it attractive and
fascinating to scientific minds.

The evidence in support of the nebulous origin of the solar system, if
not conclusive, is of much weight and importance. The remarkable harmony
with which the orbs of the system perform their motions is strongly
indicative of their common origin and that their evolution occurred in
subordination to the law of universal gravitation. The following are the
characteristic points in favour of this theory:--

1. All the planets revolve round the Sun in the same direction, and they
all occupy nearly the same plane.

2. Their satellites, with the exception of those of Uranus and Neptune,
perform their revolutions in obedience to the same law.

3. The rotation on their axes of the Sun, planets, and satellites is in
the same direction as their orbital motion.

Between the orbits of Mars and Jupiter there revolves a remarkable group
of small planets or planetoids. On account of the absence of a planet in
this region, where, according to the laws of planetary distances, one
ought to be found, the existence of those small bodies was suspected for
some years prior to their discovery. The first was detected by Piazzi at
Palermo in 1801; two others were discovered by Olbers in 1802 and 1807,
and one by Harding in 1804. For some time it was believed that no more
planetoids existed, but in 1845 a fifth was detected by Hencke, and from
that year until now upwards of 300 of those small bodies have been
discovered. Their magnitudes are of varied extent; the diameter of the
largest is believed not to exceed 450 miles, and that of the smaller
ones from twenty to thirty miles. It was surmised at one time, when only
a few of those bodies were known, that they were the fragments of a
planet which met with some terrible catastrophe; but since the discovery
of so many other planetoids this theory cannot be maintained. According
to the nebular hypothesis, these bodies are the consolidated portions of
a nebulous ring which remained separate instead of having coalesced into
one mass so as to form a planet. The uniform condensation of the ring
would result in the formation of a multitude of small planets similar to
what are found between the orbits of Mars and Jupiter. In Saturn's ring
we have a remarkable instance of annular consolidation in which the form
of the ring has been preserved. The ring is believed to consist of
myriads of minute bodies, each of which travels in an orbit of its own
as it pursues its path round the planet; the close approximation and
exceeding minuteness of those moving objects create the appearance of a
solid continuous ring.

Though, by means of the nebular hypothesis, it is impossible to explain
all the phenomena associated with the motions of the orbs which enter
into the structure of the solar system, yet this does not detract much
from the merits of the theory, the fundamental principles of which are
based upon the evolution of the solar system from a rotating nebula.
The retrograde motions of the satellites of Uranus and Neptune, the
velocity of the inner Martian moon, and other abnormalities in the
system, have not as yet been explained, but doubtless there are reasons
by which those peculiarities can be accounted for if they were only
known, '_felix qui potuit cognoscere causas omnium rerum_.'

No attempt has been made to supplant the nebular hypothesis by any other
theory of cosmical evolution. Modern investigations and discoveries have
strengthened its position, and at present it is the only means by which
we can account for the existence of the visible material universe by
which we are surrounded.

In the days when Milton lived--three hundred years ago--the nocturnal
heavens presented the same appearance to an observer as they do at the
present time. The stars pursued their identical paths, and looked down
upon the Earth with the same aspect of serene tranquillity, regardless
of the vicissitudes which affect the inhabitants of this terrestrial
sphere. The constellations that adorn the celestial vault duly appeared
in their seasons,

                    and in the ascending scale
    Of Heaven the stars that usher evening rose.--iv. 354-55.

The winter glories of Orion, the scintillating brilliancy of Sirius, and
the spangled firmament, bearing no impress of change or variation which
would lead one to conclude that the heavens were other than eternal,
attracted then, as now, the admiration of beholders.

Apart from the orbs which constitute the solar system, little was known
of the sidereal heavens beyond the visual effect created by the
nocturnal aspect of the star-lit sky. Though ancient philosophers
hazarded an opinion that the stars were suns, they received but scant
attention from early astronomers, by whom they were merely regarded as
convenient fixed points which enabled them to determine with greater
accuracy the positions of the planets and the paths traced out by them
in the heavens. The Ptolemaists, who believed in the diurnal revolution
of the spheres, assigned to the stars a very subordinate place in their
cosmology, which was the one adopted by Milton; and although Copernicus
relegated them to their proper location in space, yet he had no clear
conception of a universe of stars. Tycho Brahé, who declined to accept
the Copernican theory, disbelieved that the stars were suns, and
Galileo, who discovered the stellar nature of the Milky Way, remarked
that the stars were not illumined by the Sun's rays in the same manner
that the planets are, but expressed no opinion with regard to their
physical constitution. It is only within the past fifty years that proof
has been obtained of the real nature of the stars. By the spectroscopic
analysis of their light it has been ascertained that the elements of
matter which enter into their composition exist in a condition similar
to what is found in the Sun. The stars are therefore suns, many of them
surpassing in magnitude and brilliancy the great luminary of our
system.

Though Milton makes frequent allusion to the magnificence of the starry
heavens, we have no evidence that he regarded the stars as suns, nor
does he refer to them as such in any part of his poem.[12] What
impressed him most was their number and brilliancy, to which reference
is made in the following passages:

    About him all the Sanctities of Heaven
    Stood thick as stars.--iii. 60-61.

    And sowed with stars the Heavens thick as a field.--vii. 358.

    Amongst innumerable stars, that shone
    Stars distant, but nigh hand seemed other worlds.--iii. 564-65.

                                            her reign
    With thousand lesser lights dividual holds,
    With thousand thousand stars, that then appeared
    Spangling the hemisphere.--vii. 381-84.

Milton describes the number of the fallen angels as

                              an host
    Innumerable as the stars of night.--v. 744-45,

and the attention of Satan is directed by the archangel Uriel to the
multitude of stars formed from the chaotic elements of matter:

    Numberless as thou seest, and how they move;
    Each had his place appointed, each his course;
    The rest in circuit walls this universe.--iii. 719-21.



Though Milton was doubtless familiar with the leading orbs of the
firmament and knew their names, and the constellations in which they are
situated, yet he makes no direct allusion to any of them in his poem.
Neither Arcturus, which is mentioned in the Book of Job, nor Sirius,
which attracted the attention of Homer, who compared the brightness of
Achilles' armour to the dazzling brilliancy of the dog-star, finds a
place in 'Paradise Lost.' And yet the superior magnitude and brilliancy
of some stars when compared with those of others did not escape Milton's
observation when, in describing the lofty eminence of Satan in heaven,
prior to his fall, he represents him as

                      brighter once amidst the host
    Of angels than that star the stars among.--vii. 132-33.

There is but one star to which Milton makes individual allusion, and,
though not of any conspicuous brilliancy, yet it is one of much
importance to astronomers--

            the fleecy star that bears
    Andromeda far off Atlantic seas
    Beyond the horizon.--iii. 558-60.

This is Alpha Arietis, the first point in the constellation of that
name, which signifies the Ram, and from which the right ascensions of
the stars are measured on the celestial sphere. In the time of
Hipparchus the ecliptic intersected the celestial equator in Aries,
which indicated the commencement of the astronomical year and the
occurrence of the vernal equinox; but, owing to precession, this point
is now 30° westward of Aries and in the constellation Pisces. The star
was called Hamal by the Arabs, signifying a sheep, and the animal is
represented as looking backwards. Manilius writes:--

    First Aries, glorious in his golden wool,
    Looks back and wonders at the mighty Bull.

Aries is associated with the legend of the Golden Fleece, in quest of
which Jason and his valiant crew sailed in the ship 'Argo.' In the
autumn, Andromeda is situated above Aries, and would seem to be borne by
the latter, which accounts for Milton's description of the relative
positions of those two constellations.

Milton alludes to the starry sphere in several passages in his poem, and
also mentions the starry pole above which he soared in imagination up to
the Empyrean or Heaven of Heavens. His contemplation of the Galaxy must
have impressed his mind with the magnitude and extent of the sidereal
universe, for he was aware that this luminous zone which encircles the
heavens consists of myriads of stars, so remote as to be incapable of
definition by unaided vision. Milton's description of this vast
assemblage of stars is worthy of its magnificence, and the purpose with
which he poetically associates this glorified highway testifies to the
sublimity of his thoughts and to the originality of his genius. In those
parts of his poem in which he describes the glories of the celestial
regions, and instances the beautiful phenomena associated with the
individual orbs of the firmament, we are able to perceive with what
exquisite delight he beheld them all.

The invention of the telescope, and the important discoveries made by
Kepler, Galileo, and Newton in the seventeenth century, were the means
of effecting a rapid advance in the science of astronomy; but that
branch of it known as sidereal astronomy was not then in existence. The
star depths, owing to inadequate telescopic power, remained unexplored,
and the secrets associated with those distant regions were inviolable,
and lay beyond the reach of human knowledge. The physical constitution
of the stars was unknown, nor was it ascertained with any degree of
certainty that they were suns. The knowledge possessed by astronomers in
those days was but meagre compared with what is now known of the
sidereal heavens. Milton's astronomical knowledge, we find, was
commensurate with what was known of the stellar universe, and this he
has conspicuously displayed in his poem.




CHAPTER VIII

DESCRIPTION OF CELESTIAL OBJECTS MENTIONED IN 'PARADISE LOST'


THE SUN

The surpassing splendour of the Sun, as compared with that of any of the
other orbs of the firmament, is not more impressive than his stupendous
magnitude, and the important functions which it is his prerogative to
fulfil. Situated at the centre of our system--of which he may be
regarded as 'both eye and soul'--the orb has a diameter approaching
1,000,000 miles, and a mass 750 times greater than that of all the
planets combined. These, by his attractive power, he retains in their
several paths and orbits, and even far distant Neptune acknowledges his
potent sway. With prodigal liberality he dispenses his vast stores of
light and heat, which illumine and vivify the worlds circling around
him, and upon the constant supply of which all animated beings depend
for their existence. Deprived of the light of the Sun, this world would
be enveloped in perpetual darkness, and we should all miserably perish.

The Sun is distant from the Earth about 93,000,000 miles. His diameter
is 867,000 miles, or nearly four times the extent of the radius of the
Moon's orbit. The mass of the orb exceeds that of the Earth 330,000
times, and in volume 1,305,000 times. The Sun is a sphere, and rotates
on his axis from west to east in 25 days 8 hours. The velocity of a
point at the solar equator is 4,407 miles an hour. The density of the
Sun is only one-fourth that of the Earth, or, in other words, bulk for
bulk, the Earth is four times heavier than the Sun. The force of gravity
at the Sun's surface is twenty-seven times greater than it is on the
Earth; it would therefore be impossible for beings constituted as we are
to exist on the solar surface.

The dazzling luminous envelope which indicates to the naked eye the
boundary of the solar disc is called the PHOTOSPHERE. It is most
brilliant at the centre of the Sun, and diminishes in brightness towards
the circumference, where its luminosity is but one-fourth that of the
central portion of the disc. The photosphere consists of gaseous vapours
or clouds, of irregular form and size, separated by less brilliant
interstices, and glowing white with the heat derived from the interior
of the Sun. In the telescope the photosphere is not of uniform
brilliancy, but presents a mottled or granular appearance, an effect
created by the intermixture of spaces of unequal brightness. Small
nodules of intense brilliance, resembling 'rice-grains,' but which,
according to Nasmyth, are of a willow-leaf shape with pointed
extremities, which form a network over portions of the photosphere, are
sprinkled profusely over a more faintly luminous background. These
'grains' consist of irregular rounded masses, having an area of several
hundred miles. By the application of a high magnifying power they can be
resolved into 'granules'--minute luminous dots which constitute
one-fifth of the Sun's surface and emit three-fourths of the light. This
granulation is not uniform over the surface of the photosphere; in some
parts it is indistinct, and appears to be replaced by interlacing
filamentous bands, which are most apparent in the penumbræ of the spots
and around the spots themselves. The 'granules' are the tops of
ascending masses of intensely luminous vapour; the comparatively dark
'pores' consist of similar descending masses, which, having radiated
their energy, are returning to be again heated underneath the surface of
the photosphere.

In certain regions of the photosphere several dark patches are usually
visible, which are called 'sun-spots.' At occasional times they are
almost entirely absent from the solar disc. It has been observed that
they occupy a zone extending from 10° to 35° north and south of the
solar equator, but are not found in the equatorial and polar regions of
the Sun. A sun-spot is usually described as consisting of an irregular
dark central portion, called the _umbra_; surrounding it is an edging or
fringe less dark, consisting of filaments radiating inwards called the
_penumbra_. Within the umbra there is sometimes seen a still darker
spot, called the _nucleus_. The umbra is generally uniformly dark, but
at times filmy luminous clouds have been observed floating over it. The
nucleus is believed to be the orifice of a tubular depression in the
floor of the umbra, prolonged downwards to an unknown depth. The
penumbra is brightest at its inner edge, where the filaments present a
marked contrast when compared with the dark cavity of the umbra which
they surround and overhang. Sometimes lengthened processes unite with
those of the opposite side and form bands and 'bridges' across the
umbra. The darkest portion of the penumbra is its external edge, which
stands out conspicuously against the adjoining bright surface of the
Sun. One penumbra will sometimes enclose several umbræ whilst the nuclei
may be entirely wanting.

[Illustration: FIG. 6.--A Sun-spot magnified.

(_Janssen._)]

Sun-spots usually appear in groups; large isolated spots are of rare
occurrence, and are generally accompanied by several smaller ones of
less perfect formation. The exact moment of the origin of a sun-spot
cannot be ascertained, because it arises from an imperceptible point; it
grows very rapidly, and often attains its full size in a day.

Prior to its appearance there is an unusual disturbance of the solar
surface over the site of the spot: luminous ridges, called _faculæ_, and
dark 'pores' become conspicuous, between which greyish patches appear,
that seem to lie underneath a thin layer of the photosphere; this is
rapidly dispelled and a fully formed spot comes into view. When a
sun-spot has completed its period of existence, the photospheric matter
overwhelms the penumbra, and rushes into the umbra, which it
obliterates, causing the spot to disappear. The duration of sun-spots is
subject to considerable variation; some last for weeks or months, and
others for a few days or hours. A spot when once fully formed maintains
its shape, which is usually rounded, until the period of its breaking
up. Spots of long duration rotate with the Sun. Those which become
visible at the edge of the Sun's limb have been observed to travel
across his disc in less than a fortnight, disappearing at the margin of
the opposite limb; afterwards, if sufficiently long-lived, they have
reappeared in twelve or thirteen days on the surface of the orb where
first observed. It was by observation of the spots that the period of
the axial rotation of the Sun became known.

Sun-spots vary very much in size--some are only a few hundred miles in
width, whilst others have a diameter of 40,000 or 50,000 miles or
upwards. In some instances the umbra alone has a breadth of 20,000 or
30,000 miles--three times the extent of the diameter of the Earth. Spots
of this size are visible to the naked eye when the Sun is partially
obscured by fog, or when his brilliancy is diminished by vapours near
the horizon. A year seldom passes without the occurrence of several of
such spots being recorded. The largest sun-spot ever observed had a
diameter of about 150,000 miles. A group of spots, including their
penumbræ, will occupy an area of many millions of square miles.

By long observation it has been ascertained that sun-spots increase and
diminish in number with periodical regularity, and that a maximum
sun-spot period occurs at the end of each eleven years. When spots are
numerous on the Sun's disc there is great disturbance of the solar
surface, accompanied by fierce rushes of intensely heated gases. This
solar activity is known to influence terrestrial magnetism by causing a
marked oscillation of the magnetic needle, and giving rise to so-called
'magnetic storms,' accompanied by magnificent displays of auroræ, with
variations in electrical earth-currents. It would therefore appear that
sun-spots have a pronounced effect upon magnetic terrestrial phenomena,
but how this is produced remains unknown.

Besides sun-spots, there are seen on the solar disc bright flocculent
streaks or ridges of luminous matter called _faculæ_; they are found
over the whole surface of the Sun, but are most numerous near the limb
and in the immediate vicinity of the spots. They have been compared to
immense waves--vast upheavals of photospheric matter, indicative of
enormous pressure, and often extending in length for many thousands of
miles.

Nearly all observers have arrived at the conclusion that sun-spots are
depressions or cavities in the photosphere, but considerable difference
of opinion exists as to how they are formed. The most commonly accepted
theory is that they are caused by the pressure of descending masses of
vapour having a reduced temperature, which absorb the light and prevent
it reaching us. Our knowledge of the Sun is insufficient to admit of any
accurate conclusion on this point; though we are able to perceive that
the surface of the orb is in a state of violent agitation and perpetual
change, yet his great distance and intense luminosity prevent our
capability of perceiving the ultimate minuter details which go to form
the _texture_ of the solar surface. 'Bearing in mind that a second of
arc on the Sun represents 455 miles, it follows that an object 150 miles
in diameter is about the _minimum visible_ even as a mere mathematical
point, and that anything that is sufficiently large to give the
slightest impression of shape and extension of surface must have an
area of at least a quarter of a million square miles; ordinarily
speaking, we shall not gather much information about any object that
covers less than a million.'[13] Since the British Islands have only an
area of 120,700 square miles, it is evident that on the surface of the
Sun there are many phenomena and physical changes occurring which escape
our observation. Though the changes which occur in the spots and faculæ
appear to be slow when observed through the telescope, yet in reality
they are not so. Tremendous storms and cyclones of intensely heated
gases, which may be compared to the flames arising from a great furnace,
sweep over different areas of the Sun with a velocity of hundreds of
miles an hour. Vast ridges and crests of incandescent vapour are
upheaved by the action of internal heat, which exceeds in intensity the
temperature at which the most refractory of terrestrial substances can
be volatilised; and downrushes of the same photospheric matter take
place after it has parted with some of its stores of thermal energy.
Sun-spots of considerable magnitude have been observed to grow rapidly
and then disappear in a very short period of time; occasionally a spot
is seen to divide into two or more portions, the fragments flying
asunder with a velocity of not less than 1,000 miles an hour. It is by
these upheavals and convulsions of the solar atmosphere that the light
and heat are maintained which illumine and vivify the worlds that
gravitate round the Sun.

During total eclipses of the Sun, several phenomena become visible which
have enabled astronomers to gain some further knowledge of the nature of
the solar appendages. The most important of these is the CHROMOSPHERE,
which consists of layers of incandescent gases that envelop the
photosphere and completely surround the Sun. Its average depth is from
5,000 to 6,000 miles, and when seen during an eclipse is of a beautiful
rose colour, resembling a sheet of flame. As seen in profile at the edge
of the Sun's disc, it presents an irregular serrated appearance, an
effect created by the protuberance of luminous ridges and
processes--masses of flame which arise from over its entire surface. The
chromosphere consists chiefly of glowing hydrogen, and an element called
_helium_, which has been recently discovered in a terrestrial substance
called cleveite; there are also present the vapours of iron, calcium,
cerium, titanium, barium, and magnesium. From the surface of this ocean
of fire, jets and pointed spires of flaming hydrogen shoot up with
amazing velocity, and attain an altitude of ten, twenty, fifty, and even
one hundred thousand miles in a very short period of time. They are,
however, of an evanescent nature, change rapidly in form and appearance,
and often in the course of an hour or two die down so as not to be
recognisable. These _prominences_, as they are called, have been divided
into two classes. Some are in masses that float like clouds in the
atmosphere, which they resemble in form and appearance; they are
usually attached to the chromosphere by a single stem, or by slender
columns; occasionally they are entirely free. These are called
_quiescent_ prominences; they consist of clouds of hydrogen, and are of
more lasting duration than the other variety, called _eruptive_ or
metallic prominences. The latter are usually found in the vicinity of
sun-spots, and, besides hydrogen, contain the vapours of various metals.
They are of different forms, and present the appearance of filaments,
spikes, and jets of liquid fire; others are pyramidal, convoluted, and
parabolic.

These outbursts, bending over like the jets from a fountain, and
descending in graceful curves of flame, ascend from the surface of the
chromosphere with a velocity often exceeding 100 miles in a second, and
frequently reach an enormous height, but are of transient duration. They
are closely connected with sun-spots, and are evidence of the tremendous
forces that are in action on the surface of the Sun.

The CORONA is an aureole of light which is seen to surround the Sun
during a total eclipse. It is an impressive and beautiful phenomenon,
and is only visible when the Sun is concealed behind the dark body of
the Moon. Professor Young gives the following graphic description of the
corona: 'From behind it [the Moon] stream out on all sides radiant
filaments, beams, and sheets of pearly light, which reach to a distance
sometimes of several degrees from the solar surface, forming an
irregular stellate halo, with the black globe of the Moon in its
apparent centre. The portion nearest the Sun is of dazzling brightness,
but still less brilliant than the prominences, which blaze through it
like carbuncles. Generally this inner corona has a pretty uniform
height, forming a ring three or four minutes of arc in width, separated
by a somewhat definite outline from the outer corona, which reaches to a
much greater distance and is far more irregular in form. Usually there
are several "rifts," as they have been called, like narrow beams of
darkness, extending from the very edge of the Sun to the outer night,
and much resembling the cloud shadows which radiate from the Sun before
a thundershower. But the edges of these rifts are frequently curved,
showing them to be something else than real shadows. Sometimes there are
narrow bright streamers as long as the rifts, or longer. These are often
inclined, or occasionally even nearly tangential to the solar surface,
and frequently are curved. On the whole, the corona is usually less
extensive and brilliant over the solar poles, and there is a
recognisable tendency to accumulation above the middle latitudes, or
spot zones; so that, speaking roughly, the corona shows a disposition to
assume the form of a quadrilateral or four-rayed star, though in almost
every individual case this form is greatly modified by abnormal
streamers at some point or other.' The corona surrounds the Sun and its
other envelopes to a depth of many thousands of miles. It consists of
various elements which exist in a condition of extreme tenuity;
hydrogen, helium, and a substance called coronium appear to predominate,
whilst finely divided shining particles of matter and electrical
discharges resembling those of an aurora assist in its illumination.

[Illustration: FIG. 7.--The Corona during the Eclipse of May 1883.]

We possess no knowledge of the physical structure of the interior of the
Sun, nor have we any terrestrial analogy to guide us as to how matter
would behave when subjected to such conditions of extreme temperature
and pressure as exist in the interior of the orb. Yet we are justified
in concluding that the Sun is mainly a gaseous sphere which is slowly
contracting, and that the energy expended in this process is being
transformed into heat so extreme as to render the orb a great fountain
of light.

Milton in his poem makes more frequent allusion to the Sun than to any
of the other orbs of the firmament, and, in all his references to the
great luminary, describes him in a manner worthy of his unrivalled
splendour, and of his supreme importance in the system which he upholds
and governs. After having alighted on Mount Niphates, Satan is described
as looking

    Sometimes towards Heaven and the full-blazing Sun,
    Which now sat high in his meridian tower.--iv. 29-30.

He then addresses him thus:--

    O thou that with surpassing glory crowned,
    Look'st from thy sole dominion like the god
    Of this new World--at whose sight all the stars
    Hide their diminished heads--to thee I call,
    But with no friendly voice, and add thy name,
    O Sun, to tell thee how I hate thy beams,
    That bring to my remembrance from what state
    I fell, how glorious once above thy sphere.--iv. 32-39.

On another occasion:--

    The golden Sun in splendour likest Heaven
    Allured his eye.--iii. 572-73.

In describing the different periods of the day, Milton seldom fails to
associate the Sun with these times, and rightly so, since they are
brought about by the apparent diurnal journey of the orb across the
heavens. Commencing with morning, he says:--

                                    Meanwhile,
    To re-salute the world with sacred light,
    Leucothea waked, and with fresh dews embalmed
    The Earth.--xi. 133-36.

    Soon as they forth were come to open sight
    Of day-spring, and the Sun--who, scarce up-risen,
    With wheels yet hovering o'er the ocean-brim,
    Shot parallel to the Earth his dewy ray,
    Discovering in wide landskip all the east
    Of Paradise and Eden's happy plains.--v. 138-43

                          or some renowned metropolis
    With glistering spires and pinnacles adorned,
    Which now the rising Sun gilds with his beams.--iii. 549-51.

                      while now the mounted Sun
    Shot down direct his fervid rays, to warm
    Earth's inmost womb.--v. 300-302.

                                  for scarce the Sun
    Hath finished half his journey, and scarce begins
    His other half in the great zone of Heaven.--v. 558-60.

    To sit and taste, till this meridian heat
    Be over, and the Sun more cool decline.--v. 369-70.

    And the great Light of Day yet wants to run
    Much of his race, though steep. Suspense in Heaven,
    Held by thy voice, thy potent voice he hears,
    And longer will delay, to hear thee tell
    His generation, and the rising birth
    Of Nature from the unapparent deep.--vii. 98-103.

The declining day and approach of evening are described as follows:--

    Meanwhile in utmost longitude, where Heaven
    With Earth and Ocean meets, the setting Sun
    Slowly descended, and with right aspect
    Against the eastern gate of Paradise
    Levelled his evening rays.--iv. 539-43.

                            the Sun now fallen
    Beneath the Azores; whether the Prime Orb,
    Incredible how swift, had thither rolled
    Diurnal, or this less volubil Earth,
    By shorter flight to the east, had left him there
    Arraying with reflected purple and gold
    The clouds that on his western throne attend.--iv. 591-97.

                                  the parting Sun
    Beyond the Earth's green Cape and verdant Isles
    Hesperian sets, my signal to depart.--viii. 630-32.

    Now was the Sun in western cadence low
    From noon, and gentle airs due at their hour
    To fan the Earth now waked, and usher in
    The evening cool.--x. 92-95.

                                      for the Sun,
    Declined, was hasting now with prone career
    To the Ocean Isles, and in the ascending scale
    Of Heaven the stars that usher evening rose.--iv. 352-55.

In the combat between Michael and Satan, which ended in the overthrow of
the rebel angels, Milton, in his description of their armour, says:--

                  two broad suns their shields
    Blazed opposite.--vi. 305-306,

and in describing the faded splendour of the ruined Archangel, the poet
compares him to the Sun when seen under conditions which temporarily
deprive him of his dazzling brilliancy and glory:--

                        as when the Sun new-risen
    Looks through the horizontal misty air
    Shorn of his beams, or, from behind the Moon
    In dim eclipse, disastrous twilight sheds
    On half the nations, and with fear of change
    Perplexes monarchs.--i. 594-99.

This passage affords us an example of the sublimity of Milton's
imagination and of his skill in adapting the grandest phenomena in
Nature to the illustration of his subject.


THE MOON

The Moon is the Earth's satellite, and next to the Sun is the most
important of the celestial orbs so far as its relations with our globe
are concerned. Besides affording us light by night, the Moon is the
principal cause of the ebb and flow of the tide--a phenomenon of much
importance to navigators. The Moon is almost a perfect sphere, and is
2,160 miles in diameter. The form of its orbit is that of an ellipse
with the Earth in the lower focus. It revolves round its primary in 27
days 7 hours, at a mean distance of 237,000 miles, and with a velocity
of 2,273 miles an hour. Its equatorial velocity of rotation is 10 miles
an hour. The density of the Moon is 3·57 that of water, or 0·63 that of
the Earth; eighty globes, each of the weight of the Moon, would be
required to counterbalance the weight of the Earth, and fifty globes of
a similar size to equal it in dimensions. The orb rotates on its axis in
the same period of time in which it accomplishes a revolution of its
orbit; consequently the same illumined surface of the Moon is always
directed towards the Earth. To the naked eye the Moon appears as large
as the Sun, and it very rapidly changes its form and position in the
sky. Its motions, which are of a very complex character, have been for
many ages the subject of investigation by mathematicians and
astronomers, but their difficulties may now be regarded as having been
finally overcome.

The phases of the Moon are always interesting and very beautiful. The
orb is first seen in the west, after sunset, as a delicate slender
crescent of pale light; each night it increases in size, whilst it
travels eastward, until it attains the figure of a half moon; still
growing larger as it pursues its course, it finally becomes a full
resplendent globe, rising about the time that the Sun sets and situated
directly opposite to him. Then, in a reverse manner, after full moon, it
goes through the same phases, until, as a slender crescent, it becomes
invisible in the solar rays; afterwards to re-appear in a few days, and,
in its monthly round, to undergo the same cycle of changes. The phases
of the Moon depend upon the changing position of the orb with regard to
the Sun. The Moon shines by reflected light derived from the Sun, and as
one half of its surface is always illumined and the other half totally
dark, the crescent increases or diminishes when, by the Moon's change of
position, we see more or less of the bright side. Visible at first as a
slender crescent near the setting Sun, the angular distance from the orb
and the width of the crescent increase daily, until, at the expiration
of seven days, the Moon is distant one quarter of the circumference of
the heavens from the Sun. The Moon is then a semi-circle, or in
quadrature. At the end of other seven days, the distance of the Moon
from the Sun is at its greatest--half the circumference of its orbit. It
is then visible as a circular disc and we behold the orb as full moon.
The waning Moon, as it gradually decreases, presents the same aspects
reversed, and, finally, its slender crescent disappears in the Sun's
rays. The convex edge of the crescent is always turned towards the Sun.
The rising of the Moon in the east and its setting in the west is an
effect due to the diurnal rotation of the Earth on her axis, but the orb
can be perceived to have two motions besides: one from west to east,
which carries it round the heavens in 29·53 days, and another from north
to south. The west to east motion is steady and continuous, but, owing
to the Sun's attractive force, the Moon is made to swerve from its path,
giving rise to irregularities of its motion called PERTURBATIONS. The
most important of these is the _annual equation_, discovered by Tycho
Brahé--a yearly effect produced by the Sun's disturbing influence as the
Earth approaches or recedes from him in her orbit; another irregularity,
called the _evection_, is a change in the eccentricity of the lunar
orbit, by which the mean longitude of the Moon is increased or
diminished. _Elliptic inequality_, _parallactic inequality_, the
_variation_, and _secular acceleration_, are other perturbations of the
lunar motion, which depend directly or indirectly on the attractive
influence of the Sun and the motion of the Earth in her orbit.

As the plane of the Moon's orbit is inclined at an angle of rather more
than 5° to the ecliptic, it follows that the orb, in its journey round
the Earth, intersects this great circle at two points called the
'Nodes.' When crossing the ecliptic from south to north the Moon is in
its ascending node, and when crossing from north to south in its
descending node. In December the Moon reaches the most northern point of
its course, and in June the southernmost. Consequently we have during
the winter nights the greatest amount of moonlight, and in summer the
least. In the evenings the moonlight is least in March and greatest in
September, when we have what is called the Harvest Moon.

The telescopic appearance of the Moon is very interesting and beautiful,
especially if the orb is observed when waxing and waning. As no aqueous
vapour or cloud obscures the lunar surface, all its details can be
perceived with great clearness and distinctness. Indeed, the topography
of the Moon is better known than that of the Earth, for the whole of its
surface has been mapped and delineated with great accuracy and
precision. The Moon is in no sense a duplicate of its primary, and no
analogy exists between the Earth and her satellite. Evidence is wanting
of the existence of an atmosphere surrounding the Moon; no clouds or
exhalations can be perceived, and no water is believed to exist on the
lunar surface. Consequently there are no oceans, seas, rivers, or lakes;
no fertile plains or forest-clad mountains, such as are found upon the
Earth. Indeed, all the conditions essential for the support and
maintenance of organic life by which we are surrounded appear to be
nonexistent on the Moon. Our satellite has no seasons; its axial
rotation is so slow that one lunar day is equal in length to fourteen of
our days; this period of sunshine is succeeded by a night of similar
duration. The alternation of such lengthened days and nights subjects
the lunar surface to great extremes of heat and cold.

When viewed with a telescope, the surface of the Moon is perceived to
consist of lofty mountain chains with rugged peaks, numerous extinct
volcanoes called crater mountains, hills, clefts, chasms, valleys, and
level plains--a region of desolation, presenting to our gaze the
shattered and upturned fragments of the Moon's crust, convulsed by
forces of a volcanic nature which have long since expended their
energies and died out. The mountain ranges on the Moon resemble those of
the Earth, but they have a more rugged outline, and their peaks are more
precipitous, some of them rising to a height of 20,000 feet. They are
called the Lunar Alps, Apennines, and Cordilleras, and embrace every
variety of hill, cliff, mound, and ridge of comparatively low
elevation. The plains are large level areas, which are situated on
various parts of the lunar surface; they are of a darker hue than the
mountainous regions by which they are surrounded, and were at one time
believed to be seas. They are analogous to the prairies, steppes, and
deserts of the Earth.

_Valleys._--Some of these are of spacious dimensions; others are narrow,
and contract into gorges and chasms. Clefts or rills are long cracks or
fissures of considerable depth, which extend sometimes for hundreds of
miles across the various strata of which the Moon's crust is composed.

The characteristic features of the Moon's surface are the crater
mountains: they are very numerous on certain portions of the lunar disc,
and give the Moon the freckled appearance which it presents in the
telescope, and which Galileo likened to the eyes in the feathers of a
peacock's tail. They are believed to be of volcanic origin, and have
been classified as follows: 'Walled plains, mountain rings, ring plains,
crater plains, craters, craterlets, and crater cones.' Upwards of 13,000
of these mountains have been enumerated, and 1,000 are known to have a
diameter exceeding nine miles. Walled plains consist of circular areas
which have a width varying from 150 miles to a few hundred yards. They
are enclosed by rocky ramparts, whilst the centre is occupied by an
elevated peak. The depth of these formations, which are often far below
the level of the Moon's surface, ranges from 10,000 to 20,000 feet.
Mountain rings, ring plains, and crater plains resemble those already
described, but are on a smaller scale; the floors of the larger ones are
frequently occupied by craters and craterlets. The latter exist in large
numbers, and some portions of the Moon's surface appear honeycombed with
them, the smaller craters resting on the sides of larger ones and
occupying the bottoms of the more extensive areas. There is no kind of
formation on the Earth's surface that can be compared with these crater
mountains, which indicate that the Moon was at one time a fiery globe
convulsed by internal forces which found an outlet in the numerous
volcanoes scattered over her surface.

The most remarkable of these volcanic mountains have been named after
distinguished men. (1) Copernicus is one of the most imposing; its
crater is 56 miles in diameter, and situated at its centre is a mountain
with six peaks 2,400 feet in height. The ring by which it is surrounded
rises 11,000 feet above the floor of the crater, and consists of
terraces believed to have been created by the partial congelation and
periodic subsidence of a lake of molten lava which occupied the enclosed
area.

(2) Tycho is one of the most magnificent and perfect of lunar volcanoes,
and is also remarkable as being a centre from which, when the Moon is
full, there radiates a number of bright streaks which extend across the
lunar surface, over mountain and valley, through ring and crater, for
many hundreds of miles. Their nature is unknown, and nothing resembling
them is found on the Earth. Tycho has a diameter of 50 miles and a
depth of 17,000 feet. The peak which rises from the floor of the crater
attains a height of 6,000 feet, and the rampart consists of a series of
terraces which give variety to the appearance of the inner wall. The
surface of the Moon round Tycho is honeycombed with small volcanoes.

(3) Clavius is one of the most extensive of the walled plains; it has a
diameter of 142 miles and an area of 16,500 square miles. The rocky
annulus which surrounds it is very lofty and precipitous, and at one
point reaches a height of 17,300 feet. Upwards of 90 craters have been
counted within this space, one of the peaks attaining to an elevation of
24,000 feet above the level floor of the plain. It is believed that the
lowest depths of this wild and precipitous region are never penetrated
by sunlight, they are so overshadowed by towering crag and fell which
intercept the solar rays; and, as there is no atmosphere to cause
reflection, they are consequently enveloped in perpetual darkness.

(4) Plato has a diameter of about 60 miles and an area of 2,700 square
miles; its central peak rises to a height of 7,300 feet. It has an
irregular rampart which is broken up into terraces averaging about 4,000
feet high; three cones, each with an elevation of from 7,000 to 9,000
feet, rest on its western border.

(5) Theophilus is the deepest of the visible craters on the Moon. It has
a diameter of 64 miles, and the inner edge of the ring rises from the
level floor to a height ranging from 14,000 to 18,000 feet. A group of
mountains occupies the centre of the area, the highest peak of which
reaches an elevation of 5,200 feet. Cyrillus and Catharina, two adjacent
craters, are each about 16,000 feet deep and connected by a wide valley.

(6) Aristarchus is the brightest spot on the Moon, and appears almost
dazzling in the telescope. The crater has a diameter of 42 miles, the
centre of which is occupied by a steep mountain. The rampart on the
western side rises to a height of 7,500 feet, on the east it becomes a
plateau which connects it with a smaller crater called Herodotus. Bright
streaks radiate from Aristarchus when there is full moon, and extend for
a considerable distance over the surface of the orb.

Though the face of the Moon has been carefully scanned for two centuries
and a half, and selenographers have mapped and delineated her features
with the utmost accuracy and precision, yet no perceptible change of a
reliable character has been perceived to occur on any part of the orb.
The surface of the hemisphere directed towards the Earth appears to be
an alternation of desert plains, craggy wildernesses, and extinct
volcanoes--a region of desolation unoccupied by any living thing, and
'upon which the light of life has never dawned.' Owing to the absence of
an atmosphere, there is neither diffuse daylight nor twilight on the
Moon. Every portion of the lunar surface not exposed to the Sun's rays
is shrouded in darkness, and black shadows can be observed fringing
prominences of silvery whiteness. If the Moon were enveloped in an
atmosphere similar to that which surrounds the Earth, the reflection and
diffusion of light among the minute particles of watery vapour which
permeate it would give rise to a gradual transition from light to
darkness; the lunar surface would be visible when not illumined by the
direct rays of the Sun, and before sunrise and after sunset, dawn and
twilight would occur as upon the Earth. But upon the Moon there is no
dawn, and the darkness of night envelops the orb until the appearance of
the edge of the Sun's disc above the horizon, then his dazzling rays
illumine the summits and loftiest peaks of the lunar mountains whilst
yet their sides and bases are wrapped in deep gloom. Since the pace of
the Sun across the lunar heavens is 28 times slower than it is with us,
there is continuous sunshine on the Moon for 304 hours, and this long
day--equal to about a fortnight of our time--is succeeded by a night of
similar duration. As there is no atmosphere overhead to diffuse or
reflect the light, the Sun shines in a pitch-black sky, and at lunar
noonday the planets and constellations can be seen displaying a
brilliancy of greater intensity than can be perceived on Earth during
the darkest night. Every portion of the Moon's surface is bleak, bare,
and untouched by any softening influences. No gentle gale ever sweeps
down her valleys or disturbs the dead calm that hangs over this world;
no cloud ever tempers the fierce glare of the Sun that pours down his
unmitigated rays from a sky of inky blackness; no refreshing shower ever
falls upon her arid mountains and plains; no sound ever breaks the
profound stillness that reigns over this realm of solitude and
desolation.

[Illustration: A PORTION OF THE MOON'S SURFACE]

As might be expected, Milton makes frequent allusion to the Moon in
'Paradise Lost,' and does not fail to set forth the distinctive charms
associated with the unrivalled queen of the firmament. The majority of
poets would most likely regard a description of evening as incomplete
without an allusion to the Moon. Milton has adhered to this sentiment,
as may be perceived in the following lines:--

                                    till the Moon,
    Rising in clouded majesty, at length
    Apparent queen, unveiled her peerless light,
    And o'er the dark her silver mantle threw.--iv. 606-609.

                                        now reigns
    Full-orbed the Moon, and with more pleasing light,
    Shadowy sets off the face of things.--v. 41-43.

The association of the Moon with the nocturnal revels and dances of
elves and fairies is felicitously expressed in the following passage:--

                                or faëry elves,
    Whose midnight revels, by a forest side
    Or fountain, some belated peasant sees,
    Or dreams he sees, while overhead the Moon
    Sits arbitress, and nearer to the Earth
    Wheels her pale course.--i. 781-86.

In contrast with this, we have Milton's description of the Moon when
affected by the demoniacal practices of the 'night-hag' who was believed
to destroy infants for the sake of drinking their blood, and applying
their mangled limbs to the purposes of incantation. The legend is of
Scandinavian origin and the locality Lapland:--

    Nor uglier follow the night-hag, when called
    In secret, riding through the air she comes,
    Lured with the smell of infant blood, to dance
    With Lapland witches, while the labouring Moon
    Eclipses at their charms.--ii. 662-66.

In his description of the massive shield carried by Satan, the poet
compares it with the full moon:--

                                his ponderous shield
    Ethereal temper, massy, large, and round,
    Behind him cast. The broad circumference
    Hung on his shoulders like the Moon.--i. 284-87.

The phases displayed by the Moon in her monthly journey round the Earth,
and which lend a variety of charm to the appearances presented by the
orb, are poetically described by Milton in the following lines:--

                      but there the neighbouring Moon
    (So call that opposite fair star) her aid
    Timely interposes, and her monthly round
    Still ending, still renewing, through mid-Heaven
    With borrowed light her countenance triform
    Hence fills and empties, to enlighten the Earth,
    And in her pale dominion checks the night.--iii. 726-32.

It is interesting to observe how aptly Milton describes the subdued
illumination of the Moon's reflected light, as compared with the
brilliant radiance of the blazing Sun, and how the distinguishing glory
peculiar to each orb is appropriately set forth in the various passages
in which they are described; their contrasted splendour enhancing rather
than detracting from the grandeur and beauty belonging to each.


THE PLANET EARTH[14]

No lovelier planet circles round the Sun than the planet Earth, with her
oceans and continents, her mountains, valleys, rivers, lakes, and
plains; surrounded by heaven's azure, radiant with the sunlight of her
day and adorned by night with countless sparkling points of gold. This
beautiful world, the abode of MAN, is of paramount importance to us, and
is the only part of the universe of which we have any direct knowledge.

The Earth may be regarded as one of the Sun's numerous family, and is
situated third in order from the refulgent orb, round which it revolves
in an elliptical orbit at a mean distance of 92,800,000 miles. The Earth
is nearest to the Sun at the end of December, and furthest away at the
beginning of July; the difference between those distances is 3,250,000
miles--the extent of the eccentricity of the planet's orbit. The figure
of the Earth is that of an oblate spheroid; it is slightly flattened at
the poles and bulges at the equator. Its polar or shortest diameter is
7,899 miles, its equatorial diameter is 7,926 miles--greater than the
other by 27 miles. The circumference of the Earth at the equator is
24,899 miles, and the total area of its surface is 197,000,000 square
miles. Its mean density is 5-1/2 times greater than that of water.

The two principal motions performed by the Earth are: (1) Rotation on
its axis; (2) its annual revolution round the Sun. The Earth always
rotates in the same manner, and in the same direction, from west to
east. As the axis of rotation corresponds with the shortest diameter of
the planet, it affords strong evidence that the Earth assumed its
present shape whilst rapidly rotating round its axis when in a fluid or
plastic condition. This would accord with the nebular hypothesis. The
ends of the Earth's axis are called the poles of the Earth; one is the
north, the other the south pole. The north pole is directed towards a
star in the Lesser Bear called the Pole Star. The south pole is directed
to a corresponding opposite part of the heavens. The Earth's axis is
inclined 63° 33´ to the plane of the ecliptic, and is always directed to
the same point in the heavens. The Earth accomplishes a revolution on
its axis in 23 hours 56 minutes 4 seconds mean solar time, which is the
length of the sidereal day. This rate of rotation is invariable. At the
equator, where the circumference of the globe exceeds 24,000 miles, the
velocity of a point on its surface is upwards of 1,000 miles an hour,
but, as the poles are approached, the tangential velocity diminishes,
and at those points it is entirely absent. The Earth accomplishes a
revolution of her orbit in 365 days 6 hours 9 minutes; in her journey
round the Sun she travels a circuit of 580,000,000 miles at an average
pace of 66,000 miles an hour. The Earth has other slight motions called
_perturbations_, which are produced by the gravitational attraction of
other members of the solar system. The most important of these is
Precession of the Equinoxes, which is caused by the attraction of the
Sun, Moon, and planets, on the protuberant equatorial region of the
globe. This attraction has a tendency to turn the Earth's axis at right
angles to her orbit, but it only results in the slow rotation of the
pole of the equator round that of the ecliptic, which is occurring at
the rate of 1° in 70 years, and will require a period of 25,868 years to
complete an entire revolution of the heavens.

The spot on Earth round which is centred the chief interest in Milton's
poem is Paradise, which was situated in the east of Eden, a district of
Central Asia. It was here where God ordained that man should first
dwell--a place created for his enjoyment and delight. Satan, after his
soliloquy on Mount Niphates, directs his way to Paradise, and arrives
first in Eden, where he beholds from a distance the Happy Garden--

    So on he fares, and to the border comes
    Of Eden, where delicious Paradise,
    Now nearer, crowns with her enclosure green,
    As with a rural mound, the champain head
    Of a steep wilderness, whose hairy sides
    With thicket overgrown, grotesque and wild,
    Access denied; and overhead upgrew
    Insuperable highth of loftiest shade,
    Cedar, and pine, and fir, and branching palm,
    A sylvan scene, and, as the ranks ascend,
    Shade above shade, a woody theatre
    Of stateliest view. Yet higher than their tops
    The verdurous wall of Paradise up-sprung;
    Which to our general sire gave prospect large
    Into his nether empire neighbouring round.
    And higher than that wall, a circling row
    Of goodliest trees, loaden with fairest fruit,
    Blossoms and fruits at once of golden hue,
    Appeared, with gay enamelled colours mixed;
    On which the Sun more glad impressed his beams
    Than in fair evening cloud, or humid bow,
    When God hath showered the Earth: so lovely seemed
    That landskip. And of pure now purer air
    Meets his approach, and to the heart inspires
    Vernal delight and joy, able to drive
    All sadness but despair. Now gentle gales,
    Fanning their odoriferous wings, dispense
    Native perfumes, and whisper whence they stole
    Those balmy spoils.--iv. 131-59.

Satan, having gained admission to the Garden by overleaping the tangled
thicket of shrubs and bushes which formed an impenetrable barrier and
prevented any access to the enclosure within, he flew up on to the Tree
of Life--

    Beneath him, with new wonder, now he views,
    To all delight of human sense exposed,
    In narrow room Nature's whole wealth; yea, more!--
    A Heaven on Earth: for blissful Paradise
    Of God the garden was, by Him in the east
    Of Eden planted, Eden stretched her line
    From Auran eastward to the royal towers
    Of great Seleucia, built by Grecian kings,
    Or where the sons of Eden long before
    Dwelt in Telassar. In this pleasant soil
    His far more pleasant garden God ordained.
    Out of the fertile ground he caused to grow
    All trees of noblest kind for sight, smell, taste;
    And all amid them stood the Tree of Life,
    High eminent, blooming ambrosial fruit
    Of vegetable gold; and next to life,
    Our death, the Tree of Knowledge, grew fast by--
    Knowledge of good, bought dear by knowing ill.
    Southward through Eden went a river large,
    Nor changed his course, but through the shaggy hill
    Passed underneath ingulfed; for God had thrown
    That mountain, as his garden mould, high raised
    Upon the rapid current, which, through veins
    Of porous earth with kindly thirst up-drawn,
    Rose a fresh fountain, and with many a rill
    Watered the garden; thence united fell
    Down the steep glade, and met the nether flood,
    Which from his darksome passage now appears,
    And now, divided into four main streams,
    Runs diverse, wandering many a famous realm
    And country whereof here needs no account;
    But rather to tell how, if Art could tell
    How, from that sapphire fount the crisped brooks,
    Boiling on orient-pearl and sands of gold,
    With mazy error under pendent shades
    Ran nectar, visiting each plant, and fed
    Flowers worthy of Paradise, which not nice Art
    In beds and curious knots, but Nature boon
    Poured forth profuse on hill, and dale, and plain,
    Both where the morning Sun first warmly smote
    The open field, and where the unpierced shade
    Imbrowned the noontide bowers.--iv. 205-46.

Milton's description of Paradise is not less remarkable in its way than
the lurid scenes depicted by him in Pandemonium. The versatility of his
poetic genius is nowhere more apparent than in the charming pastoral
verse contained in this part of his poem. The poet has lavished the
whole wealth of his luxuriant imagination in his description of Eden and
blissful Paradise with its 'vernal airs' and 'gentle gales,' its verdant
meads, and murmuring streams, 'rolling on orient-pearl and sands of
gold;' its stately trees laden with blossom and fruit; its spicy groves
and shady bowers, over which there breathed the eternal Spring.

In Book IX. Satan expresses himself in an eloquent apostrophe to the
primitive Earth, over which he previously wandered for seven days--

    O Earth, how like to Heaven, if not preferred
    More justly, seat worthier of gods, as built
    With second thoughts, reforming what was old!
    For what God, after better, worse would build?
    Terrestrial Heaven, danced round by other Heavens,
    That shine, yet bear their bright officious lamps,
    Light above light, for thee alone, as seems,
    In thee concentring all their precious beams
    Of sacred influence! As God in Heaven
    Is centre, yet extends to all, so thou
    Centring receiv'st from all those orbs; in thee,
    Not in themselves, all their known virtue appears,
    Productive in herb, plant, and nobler birth
    Of creatures animate with gradual life
    Of growth, sense, reason, all summed up in Man,
    With what delight I could have walked thee round,
    If I could joy in aught--sweet interchange
    Of hill and valley, rivers, woods, and plains,
    Now land, now sea, and shores with forest crowned,
    Rocks, dens, and caves.--ix. 99-118.

Though it is impossible to regard the Earth as possessing the importance
ascribed to it by the ancient Ptolemaists; nevertheless, our globe is a
great and mighty world, and appears to be one of the most favourably
situated of all the planets, being neither near the Sun nor yet very far
distant from the orb; and although, when compared with the universe, it
is no more than a leaf on a tree in the midst of a vast forest; still,
it is not the least important among other circling worlds, and
unfailingly fulfils the part allotted to it in the great scheme of
creation.


THE PLANET HESPERUS

This is the beautiful morning and evening star, the peerless planet that
ushers in the twilight and the dawn, the harbinger of day and unrivalled
queen of the evening. Venus, called after the Roman goddess of Love, and
also identified with the Greek Aphrodite of ideal beauty, is the name by
which the planet is popularly known; but Milton does not so designate
it, and the name 'Venus' is not found in 'Paradise Lost.' The ancients
called it Lucifer and Phosphor when it shone as a morning star before
sunrise, and Hesperus and Vesper when it became visible after sunset. It
is the most lustrous of all the planets, and at times its brilliancy is
so marked as to throw a distinct shadow at night.

Venus is the second planet in order from the Sun. Its orbit lies between
that of Mercury and the Earth, and in form approaches nearer to a circle
than that of any of the other planets. It travels round the Sun in
224·7 days, at a mean distance of 67,000,000 miles, and with an average
velocity of 80,000 miles an hour. Its period of rotation is unknown. By
the observation of dusky spots on its surface, it has been surmised that
the planet completes a revolution on its axis in 23-1/4 hours; but other
observers doubt this and are inclined to believe that it always presents
the same face to the Sun. When at inferior conjunction Venus approaches
nearer to the Earth than any other planet, its distance then being
27,000,000 miles. Its greatest elongation varies from 45° to 47° 12´; it
therefore can never be much more than three hours above the horizon
before sunrise, or after sunset. Venus is a morning star when passing
from inferior to superior conjunction, and during the other half of its
synodical period it is an evening star. The planet attains its greatest
brilliancy at an elongation 40° west or east of the Sun--five weeks
before and after inferior conjunction. It is at these periods, when at
its greatest brilliancy, that it casts a shadow at night.

Though so pleasing an object to the unaided eye, Venus, when observed
with the telescope, is often a source of disappointment--this is on
account of its dazzling brilliancy, which renders any accurate
definition of its surface impossible. Sir John Herschel writes: 'The
intense lustre of its illuminated part dazzles the sight, and
exaggerates every imperfection of the telescope; yet we see clearly that
its surface is not mottled over with permanent spots like the Moon; we
notice in it neither mountains nor shadows, but a uniform brightness, in
which sometimes we may indeed fancy, or perhaps more than fancy,
brighter or obscurer portions, but can seldom or never rest fully
satisfied of the fact.' It is believed that the surface of the planet is
invisible on account of the existence of a cloud-laden atmosphere by
which it is enveloped, and which may serve as a protection against the
intense glare of the sunshine and heat poured down by the not
far-distant Sun. Schröter, a German astronomer, believed that he saw
lofty mountains on the surface of the planet, but their existence has
not been confirmed by any other observer. The Sun if viewed from Venus
would have a diameter nearly half as large again as when seen from the
Earth; it is therefore probable that the planet is subjected to a much
higher temperature than what is experienced on our globe.

The phases of Venus are similar to those exhibited by the Moon, and are
caused by a change in position of the illumined hemisphere of the planet
with regard to the Earth. At superior conjunction the whole enlightened
disc of the planet is turned towards the Earth, but is invisible by
being lost in the Sun's rays. Shortly before or after it arrives at this
point, its form is gibbous, the illumined portion being less than a
circle but greater than a semi-circle. At its greatest elongation west
or east of the Sun the planet resembles the Moon in quadrature--a half
moon--and between those points and inferior conjunction it is visible
as a beautiful crescent. It becomes narrower and sharper as it
approaches inferior conjunction, until it resembles a curved luminous
thread prior to its disappearance at the conjunction. After having
passed this point it reappears on the other side of the Sun as the
morning star.

It would be only natural to imagine that this peerless orb, the most
beautiful and lustrous of the planets, upon which men have gazed with
longing admiration, and designated the emblem of 'all beauty and all
love,' should have impressed Milton's poetical imagination with its
charming appearance, and stimulated the flow of his captivating muse. He
addresses the orb as

    Fairest of Stars, last in the train of night,
    If better thou belong not to the dawn,
    Sure pledge of day, that crown'st the smiling morn
    With thy bright circlet, praise Him in thy sphere
    While day arises, that sweet hour of prime.--v. 166-70.

In these lines the poet alludes to Venus as the morning star.

In the other passages in his poem Milton associates the planet sometimes
with the morning and at other times with the evening--

    His countenance, as the Morning Star that guides
    The starry flock.--v. 708-709.

    Or if the Star of Evening and the Moon
    Haste to thy audience, Night with her will bring
    Silence, and Sleep listening to thee will watch.--vii. 104-106.

    And hence the morning planet gilds her horns.--vii. 366.

    The Sun was sunk and after him the Star
    Of Hesperus, whose office is to bring
    Twilight upon the Earth, short arbiter
    Twixt day and night.--ix. 47-50.

                      and bid haste the Evening Star
    On his hill top to light the bridal lamp.--viii. 519-20.

Milton knew of the phases of Venus and was aware that at certain times
the planet was visible in the telescope as a beautiful crescent. The
line in which he mentions her as gilding her horns is an allusion to
this appearance of Venus.


THE PLEIADES

The beautiful cluster of the Pleiades or Seven Sisters has been regarded
with hallowed veneration from time immemorial. The happy influences
believed to be shed down upon the Earth by those stars and their close
association with human destinies have rendered them objects of almost
sacred interest among the different races of mankind. In every region of
the globe and in every clime, among civilised nations and savage
fetish-worshipping tribes, the same benign influences were ascribed to
the stars which form this interesting group.

In Greek mythology they were known as the seven daughters of Atlas and
Pleione. Different versions are given of their fate. By some writers it
is said they died from grief in consequence of the death of their
sisters, the Hyades, or on account of the fate of their father, who,
for treason, was condemned by Zeus to bear on his head and hands the
vault of heaven, on the mountains of north-west Africa which bear his
name. According to others they were the companions of Diana, and, in
order to escape from Orion, by whom they were pursued, the gods
translated them to the sky.

All writers agree in saying that after their death or translation they
were transformed into stars. Their names are Alcyone, Electra, Maia,
Merope, Sterope, Taygeta, and Celaeno. The seventh Atlantid is said to
be the 'lost Pleiad,' but it can be perceived without difficulty by a
person possessing good eyesight. In the book of Job there is a beautiful
allusion to the Pleiades (chap. xxxviii.) when God speaks out of the
whirlwind and asks the patriarch to answer Him--

    Canst thou bind the sweet influences of the Pleiades, or loose the
        bands of Orion?
    Canst thou bring forth Mazzaroth in his season? or canst thou guide
        Arcturus with his sons?
    Knowest thou the ordinances of heaven? canst thou set the dominion
        thereof in the earth?

Admiral Smyth says that this noble passage is more correctly rendered as
follows:

    Canst thou bind the delightful teemings of Cheemah?
    Or the contractions of Chesil canst thou open?
    Canst thou draw forth Mazzaroth in his season
    Or Ayeesh and his sons canst thou guide?

He writes: 'In this very early description of the cardinal
constellations, _Cheemah_ denotes Taurus with the Pleiades; _Chesil_ is
Scorpio; Mazzaroth is Sirius in "the chambers of the south;" and Ayeesh
the Greater Bear, the Hebrew word signifying a _bier_, which was shaped
by the four well-known bright stars, while the three forming the tail
were considered as children attending a funeral.' The Greeks at an early
period were attracted by this cluster of stars, and Hesiod alludes to
them in his writings. One passage converted into rhyme reads as follows:

    There is a time when forty days they lie,
    And forty nights, conceal'd from human eye;
    But in the course of the revolving year,
    When the swain sharps the scythe, again appear.

Their heliacal rising was considered a favourable time for setting out
on a voyage, and their midnight culmination, which occurred shortly
after the middle of November, was celebrated by some nations with
festivals and public ceremonies. Considerable diversity of opinion
existed among the ancients with regard to the number of stars which
constitute this group. It was affirmed by some that only six were
visible, whilst others maintained that seven could be seen. Ovid writes:

    Quae septem dici, sex tamen esse solent.

Homer and Attalus mention six; Hipparchus and Aratus seven. The legend
with regard to the lost Pleiad would seem to indicate that, during a
period in the past, the star possessed a superior brilliancy and was
more distinctly visible than it is at the present time. This may have
been so, for, should it belong to the class of variable stars, there
would be a periodic ebb and flow of its light, by which its fluctuating
brilliance could be explained. When looked at directly only six stars
can be seen in the group, but should the eye be turned sideways more
than this number become visible. Several observers have counted as many
as ten or twelve, and it is stated by Kepler that his tutor, Maestlin,
was able to enumerate fourteen stars and mapped eleven in their relative
positions. With telescopic aid the number is largely increased--Galileo
observed thirty-six with his instrument and Hooke, in 1664, counted
seventy-eight. Large modern telescopes bring into view several thousand
stars in this region.

The Pleiades are situated at a profound distance in space. Their light
period is estimated at 250 years, indicating a distance of 1,500
billions of miles. Our Sun if thus far removed would be reduced to a
tenth-magnitude star. 'There can be little doubt,' says Miss Agnes
Clerke, 'that the solar brilliancy is surpassed by sixty to seventy of
the Pleiades. And it must be in some cases enormously surpassed; by
Alcyone 1,000, by Electra 480, by Maia nearly 400 times. Sirius itself
takes a subordinate rank when compared with the five most brilliant
members of a group, the real magnificence of which we can thus in some
degree apprehend.' This is the only star cluster which can be perceived
to be moving in space, or which has an ascertained common proper motion.
Its constituents form a magnificent system in which the stars bear a
mutual relationship to each other, and perform intricate internal
revolutions, whilst they in systemic union drift along through the
depths of space. There are two allusions to the Pleiades in 'Paradise
Lost.' In describing the path of the newly created Sun, Milton
introduces them as indicative of the joyfulness associated with the
birth of the Universe--

    First in his east the glorious lamp was seen,
    Regent of day, and all the horizon round
    Invested with bright rays, jocund to run
    His longitude through heaven's high road; the grey
    Dawn, and the Pleiades before him danced,
    Shedding sweet influence.--vii. 370-75.

It was believed that the Earth was created in the spring; and towards
the end of April this group rises a little before the Sun and precedes
him in his course, 'shedding sweet influences.' The ancients believed
that the good or evil influences of the stars were exercised not in the
night but during the day, when their rays mingled with those of the Sun.
The pernicious influence of the Dog-star is mentioned by Latin writers
as being most pronounced during the dog-days, at the end of summer and
commencement of autumn, the time of the heliacal rising of this star.

The other allusion to the Pleiades is in Book X., line 673, where
Milton, in describing the altered path of the Sun consequent upon the
Fall, mentions how the orb travels through Taurus with the Seven
Atlantic Sisters--the seven daughters of Atlas, the Pleiades, which are
situated on the shoulder of the animal representing this zodiacal
constellation.


THE GALAXY

The Galaxy or Milky Way is the great luminous zone encircling the
heavens, which can be seen extending across the sky from horizon to
horizon. Its diffused nebulous appearance caused the ancients much
perplexity, and many quaint opinions were hazarded as to the nature of
this celestial highway; but the mystery associated with it was not
solved until Galileo directed his newly invented telescope to this
lucent object, when, to his intense delight, he discovered that it
consists of myriads of stars--millions upon millions of suns so distant
as to be individually indistinguishable to ordinary vision, and so
closely aggregated, that their blended light gives rise to the milky
luminosity signified by its name. This stelliferous zone almost
completely encircles the sphere, which it divides into two nearly equal
parts, and is inclined at an angle of 63° to the celestial equator. In
Centaurus it divides into two portions, one indistinct and of
interrupted continuity, the other bright and well defined; these, after
remaining apart for 120°, reunite in Cygnus. The Milky Way is of
irregular outline and varies in breadth from 5° to 16°; it intersects
the equinoctial in the constellations Monoceros and Aquila, and
approaches in Cassiopeia to within 27° of the north pole of the heavens;
an equal distance intervenes between it and the south pole. Its poles
are in Coma Bernices and Cetus. The stars in the galactic tract are very
unevenly distributed; in some of its richest regions as many stars as
are visible to the naked eye on a clear night have been counted within
the space of a square degree. In other parts they are much less
numerous, and there have been observed besides, adjacent to the most
luminous portions of the zone, dark intervals and winding channels
almost entirely devoid of stars. An instance of this kind occurs in the
constellation of the Southern Cross, where there exists in a rich
stellar region a large oval-shaped dark vacuity, 8° by 5° in extent,
that appears to be almost entirely denuded of stars. In looking at it,
an impression is created that one is gazing into an empty void of space
far beyond the Milky Way. This gulf of Cimmerian darkness was called by
early navigators the Coal Sack. Similar dark spaces, though not of such
magnitude, are seen in Ophiuchus, Scorpio, and Cygnus.

The Galaxy, when viewed with a powerful telescope, is found to consist
of congeries of stars, vast stellar aggregations, great luminous tracts
resolvable into clouds of stars of overpowering magnificence, superb
clusters of various orders, and convoluted nebulous streams wandering
'with mazy error' among 'islands of light and lakes of darkness,'
resolved by the telescope into banks of shining worlds. The concourses
of stars which enter into the formation of this wonderful zone exhibit
in a marvellous degree the amazing profusion in which these orbs exist
in certain regions of space; yet those multitudes of stars perform their
motions in harmonious unison and in orderly array, and by their mutual
attraction sustain the dynamical equilibrium of this stupendous galactic
ring, the diameter of which, according to one authority, is not
traversed by light in less than 13,000 years.

[Illustration: FIG. 8.--A Portion of the Milky Way.]

Sir William Herschel, to whom we are indebted for most of what we know
of the Milky Way, commenced a series of observations in 1785 with the
object of acquiring a knowledge of the structure of the sidereal
heavens. In the accomplishment of this object, to which he devoted a
considerable part of his life, he undertook a systematic survey of that
portion of the Galaxy which is visible in the Northern Hemisphere. By a
method called star-gauging, which consisted in the enumeration of the
stars in each successive telescopic field as the instrument moved slowly
over the region under observation, he found that the depth of the star
strata could be approximately ascertained by counting the stars along
the line of vision; those were most numerous where the visual line
appeared of the greatest length and fewest in number where it was
shortest. Herschel perceived the internal structure of the Galaxy to be
exceedingly intricate and complex, and that it embraced within its
confines an endless variety of systems, clusters, and groups, branches,
sprays, arches, loops, and streaming filaments of stars, all of which
combined to form this luminous zone. 'It is indeed,' says a well-known
astronomer, 'only to the most careless glance, or when viewed through an
atmosphere of imperfect transparency, that the Milky Way seems a
continuous zone. Let the naked eye rest thoughtfully on any part of it,
and, if circumstances be favourable, it will stand out rather as an
accumulation of patches and streams of light of every conceivable
variety of form and brightness, now side by side, now heaped on each
other; again spanning across dark spaces, intertwining and forming a
most curious and complex network; and at other times darting off into
the neighbouring skies in branches of capricious length and shape which
gradually thin away and disappear.' Sir John Herschel, who was occupied
for four years at the Cape of Good Hope in exploring the celestial
regions of the Southern Hemisphere, describes the coming on of the Milky
Way as seen in his 20-foot reflector. He first remarks 'that all the
stars visible to us, whether by unassisted vision or through the best
telescopes, belong to and form part of a vast stratum or considerably
flattened and unsymmetrical congeries of stars in which our system is
deeply and eccentrically plunged; and, moreover, situated near a point
where the stratum bifurcates or spreads itself out into two sheets.' 'As
the main body of the Milky Way comes on the frequency and variety of
those masses (nebulous) increases; here the Milky Way is composed of
separate or slight or strongly connected clouds of semi-nebulous light,
and, as the telescope moves, the appearance is that of clouds passing in
a scud, as sailors call it.' The Milky Way is like sand, not strewed
evenly as with a sieve, but as if flung down by handfuls (and both hands
at once), leaving dark intervals, and all consisting of stars of the
fourteenth, sixteenth, twentieth magnitudes down to nebulosity, in a
most astonishing manner. After an interval of comparative poverty, the
same phenomenon, and even more remarkable, I cannot say it is nebulous,
it is all resolved, but the stars are inconceivably numerous and minute;
there must be millions and all almost equally massed together. Yet they
nowhere run to nuclei or clusters much brighter in the middle. Towards
the end of the seventeenth hour (Right Ascension) the globular clusters
begin to come in; they consist of stars of excessive minuteness, but
yet not more so than the ground of the Milky Way, on which not only they
appear projected, but of which it is very probable they form a part.
'From the foregoing analysis of the telescopic aspect of the Milky Way
in this interesting region, I think it can hardly be doubted that it
consists of portions differing exceedingly in distance, but brought by
the effect of projection into the same, or nearly the same, visual line;
in particular, that at the anterior edge of what we have called the main
stream, we see foreshortened a vast and illimitable area scattered over
with discontinuous masses and aggregates of stars in the manner of the
cumuli of a mackerel sky, rather than of a stratum of regular thickness
and homogeneous formation.'

The profound distance at which the stars of the Galaxy are situated in
space precludes the possibility of our obtaining any definite knowledge
of their magnitude and of the extent of the intervals by which they are
separated from each other, nor can we learn anything of the details
associated with the systems and combinations into which they enter. It
is believed that the majority of the stars in the Milky Way equal or
surpass the Sun in brilliancy and splendour. They are tenth to fifteenth
magnitude stars; now, the Sun at the distance indicated by these
magnitudes would in the telescope appear a much fainter object; he would
not reach the fifteenth magnitude. Consequently, the galactic stars are
regarded as his peers or superiors in magnitude and brilliancy. Those
myriads of suns are all in motion--in nature a stationary body is
unknown--and they are sufficiently far apart so as not to be unduly
influenced by their mutual gravitational attraction; a distance perhaps
equal to that which separates our Sun from the nearest fixed star may
intervene between each of those orbs. In the deepest recesses of the
Milky Way, Sir William Herschel was able to count 500 stars receding in
regular order behind each other; between each there existed an interval
of space, probably not less extensive than the interstellar spaces among
the stars by which we are surrounded.

The richest galactic regions in the Northern Hemisphere are found in
Perseus, Cygnus, and Aquila. Night after night could be spent in
sweeping the telescope over fields where the stars can be seen in
amazing profusion. In the interval of a quarter of an hour, Sir William
Herschel observed 116,000 stars pass before him in the telescope, and on
another occasion he perceived 258,000 stars in the space of forty-one
minutes. In the constellation of the Swan there is a region about 5° in
breadth which contains 331,000 stars. Photography reveals in a
remarkable manner the amazing richness of this stelliferous zone; the
impress of the stars on the sensitive plate of the camera, in some
instances, resembles a shower of descending snowflakes.

Though Sir William Herschel was able to fathom the Galaxy in most of its
tracts, yet there were regions which his great telescopes were unable
to penetrate entirely through. In Cepheus there is a spot where he
observed the stars become 'gradually less till they escape the eye so
that appearances here favour the idea of a succeeding more distant
clustering part.' He perceived another in Scorpio 'where, through the
hollows and deep recesses of its complicated structure, we behold what
has all the appearance of a wide and indefinitely prolonged area strewed
over with discontinuous masses and clouds of stars which the telescope
at length refuses to analyse.' The Great Cluster in Perseus, which lies
in the Milky Way, also baffled the penetrative capacity of Herschel's
instruments. We cannot help quoting Professor Nichol's description of
Herschel's observation of this remarkable object. He says: 'In the Milky
Way, thronged all over with splendours, there is one portion not
unnoticed by the general observer, the spot in the sword-hand of
Perseus. That spot shows no stars to the naked eye; the milky light
which glorifies it comes from regions to which unaided we cannot pierce.
But to a telescope of considerable power the space appears lighted up
with unnumbered orbs; and these pass on through the depths of the
infinite, until, even to that penetrating glass, they escape all
scrutiny, withdrawing into regions unvisited by its power. Shall we
adventure into these deeper retirements? Then, assume an instrument of
higher efficacy, and lo! the change is only repeated; those scarce
observed before appear as large orbs, and, behind, a new series begins,
shading gradually away, leading towards farther mysteries! The
illustrious Herschel penetrated on one occasion into this spot, until he
found himself among depths whose light could not have reached him in
much less than 4,000 years; no marvel that he withdrew from the pursuit,
conceiving that such abysses must be endless!' The Milky Way may be
regarded as a universe by itself, and our Sun as one of its myriad
stars.

Milton was aware of the stellar constitution of the Milky Way, which was
one of Galileo's discoveries. The poet gives a singularly accurate
description of this luminous path, which he glorifies as the way by
which the Deity returned up to the Heaven of Heavens after He finished
His great work of creation--

                                          So sung
    The glorious train ascending: He through Heaven,
    That opened wide her blazing portals, led
    To God's eternal house direct the way--
    A broad and ample road, whose dust is gold,
    And pavement stars, as stars to thee appear
    Seen in the Galaxy, that Milky Way
    Which nightly as a circling zone thou seest
    Powdered with stars.--vii. 573-81.


COMETS

Records of the appearance of these remarkable objects have been handed
down from earliest times; and when one of those mysterious visitors,
travelling from out the depths of space, became visible in our skies, it
was regarded with apprehension and dread as betokening the occurrence
of calamities and direful events among the nations of the Earth.

The word comet is derived from the Greek {komê}, signifying
'hair,' to which the hazy, luminous appearance of those objects bears
some resemblance. A comet consists of a bright central part called the
_nucleus_; this is surrounded by layers of nebulous matter called the
_coma_, and both combined form the _head_, from which a long appendage
extends called the _tail_. The nucleus and tail are not essential parts
of a comet, for many have been observed in which both have been wanting.
The tail is frequently very conspicuous, and presents considerable
diversity both as regards its appearance and length. In some comets it
is entirely absent, and in others it has been observed to stretch over
an arc of sixty or seventy degrees, indicating a length of 100 to 150
million miles. Sometimes it is straight, and at other times it is curved
at the extremity; it has been observed bifurcated into two branches;
and, on rare occasions, comets have been seen with two or more tails.
The tail of a comet is always directed away from the Sun; it increases
in size as the comet approaches the orb, and diminishes as it recedes
from him. This depends upon the degree of heat to which the comet is
exposed, which has the effect of driving off or evaporating some of the
matter composing the head. During the time the comet is travelling round
the Sun there is a continuous emission of this highly attenuated matter,
which is visible as the tail, but when the comet begins to recede from
the orb and reaches cooler regions of space the tail diminishes in size
as the temperature becomes reduced, and ultimately it disappears.

The appearance of a comet in the sky is often sudden and unexpected, and
one of those erratic wanderers may become visible at any time and in any
part of the heavens. It was remarked by Kepler that there are as many
comets in the sky as there are fishes in the ocean. This may or may not
be true, for they only become visible when they approach the Sun, and
the time during which they remain so does not usually exceed a few weeks
or months. Ancient astronomers were much perplexed with the motions of
comets, which appeared to be much more irregular than those of other
celestial bodies and unconformed to any known laws. Tycho Brahé believed
that comets moved in circular orbits, and Kepler imagined that they
travelled in straight lines outwards from the Sun. Newton, however, was
able to demonstrate that any conic section can be described about the
Sun consistent with the law of gravitation, and that the orbits of
comets correspond with three of the four sections into which a cone can
be divided. Consequently, they obey the laws of planetary motion. Comets
which move in ellipses of known eccentricity and return with periodical
regularity may be regarded as belonging to the solar system. Twenty of
these are known, and eleven of them have more than once passed their
perihelion. Those most familiarly known complete their periods in years
as follows:--Encke's 3·3; Swift's, 5·5; Winnecke's, 5·6; Tempel's, 6;
Brorsen's, 5·5; Faye's, 7·4; Tuttle's, 13·8, and Halley's, 76. Comets
with parabolic and hyperbolic orbits may be regarded as stray objects
which visit our system once, and depart never to return again. Besides
those already mentioned there are many comets with orbits of such marked
eccentricity that their ellipses when near perihelion cannot be
distinguished from parabolæ. The great comets of 1780, 1811, 1843, 1858,
1861, and 1882 traverse orbits approaching this form, and some of them
require hundreds and thousands of years to accomplish a circuit of their
paths.

Numerous instances of the appearance of remarkable comets have been
recorded in the annals of ancient nations. The earliest records of
comets are by the Chinese, who were careful observers of celestial
phenomena. A comet is said to have appeared at the time of the birth of
Mithridates (134 B.C.), which had a disc as large as that of the Sun; a
great comet also became visible in the heavens about the time of the
death of Julius Cæsar (44 B.C.), and another was seen in the reign of
Justinian (531 A.D.). A remarkable comet was observed in 1106, and in
1456, the year in which the Turks obtained possession of Constantinople
and threatened to overrun Europe, a great comet appeared, which was
regarded by Christendom with ominous forebodings. The celebrated
astronomer Halley was the first to predict the return of a comet.
Having become acquainted with Newton's investigations, which showed that
the forms of the orbits of comets were either parabolæ or extremely
elongated ellipses, he subjected the next great comet, which appeared in
1682, to a series of observations, calculated its orbit, and predicted
that it would return to perihelion in seventy-five or seventy-six years.
On referring to past records he discovered that a great comet appeared
in 1607, which pursued a path similar to the one traced out for his
comet, another was seen in 1531, and one in 1456. Halley perceived that
the intervals between those dates corresponded to a period of about
seventy-six years, the time which he calculated would be required for
his comet to complete a revolution of its orbit. He therefore had no
hesitation in predicting that the comet would appear again in 1758.
Halley knew that he would not be alive to witness the event, and alludes
to it in the following sentence: 'Wherefore if it should return
according to our prediction about the year 1758, impartial posterity
will not refuse to acknowledge that this was first discovered by an
Englishman.' As the time approached when the comet should be drawing
near to our system, much interest was excited among astronomers, who
would have an opportunity afforded them of testing the accuracy of
Halley's prediction. An eminent French mathematician named Clairaut
computed anew, by a method rather different to that adopted by Halley,
the retarding effect of the attraction of the planets upon the speed of
the comet, and arrived at the conclusion that it would reach perihelion
about the middle of April 1759; but, owing to unknown influences--Uranus
and Neptune not having been discovered--it might be a month before or
behind the calculated time. Clairaut made this announcement on November
14, 1758. Astronomers were now intently on the look-out for the comet,
and night after night the sky was swept by telescopes in search of the
expected visitor, which for upwards of seventy years had been pursuing
its solitary path invisible to mortal eyes. But the mental vision of the
mathematician did not fail to follow this celestial object, which was
now announced as being on the confines of our system. The comet was
first observed on December 25, 1758, it soon became conspicuous in the
heavens, and reached perihelion on March 12, 1759, a month before the
time assigned to it by Clairaut but within the limit of error allowed
for unknown influences. Halley's comet returned again in 1835, and may
be expected about the year 1911. The periodic appearance of this comet
has been traced back to the year 1305.

The celebrated comet of 1680 was noted as having been the one which
afforded Newton an opportunity of making observations which led to his
discovery that comets describe orbits round the Sun in conformity with
the different sections of a cone. The comet of 1811 was observed for
many weeks in the northern heavens as a brilliant object with a
beautiful fan-shaped tail; it completes a revolution of its orbit in
about 3,000 years. The comet of 1843 was also a splendid object. It
possessed a tail 200 million miles in length, and approached within
32,000 miles of the Sun. The heat to which it was exposed was sufficient
to volatilize the most infusible substances known to exist. Donati's
comet of 1858 will be long remembered as one of the most impressive of
celestial spectacles: its tail extended over an area of forty degrees,
and enveloped the star Arcturus, which could be seen shining through it
with undiminished brilliancy. Its period is estimated to be 2,100 years.
A great comet appeared in 1861, through the tail of which the Earth
passed without any perceptible effect having resulted. No remarkable
comets have appeared during recent years. In 1880, 1881, and 1882,
several were observed, and that of 1881 was the first successfully
photographed.

Comets consist of cosmical matter which exists in a condition of extreme
tenuity, and especially so in the coma and tail. Sir John Herschel
described them as almost spiritual in texture, and small stars have been
seen shining through their densest parts without any perceptible
diminution of their light. The nucleus is believed to be composed of a
congeries of meteoric fragments, and these, when exposed to the Sun's
heat, throw off luminous nebulous particles that are swept by some
repulsive force into space and form the appendage known as the tail.
Comets may be regarded as celestial objects that are perfectly
innocuous. Neither fear nor dread need be apprehended from their visits;
they come to please and instruct, not to injure or destroy.

Milton does not fail to introduce into his poem several allusions to
comets, and in doing so expresses the ideas and sentiments which in his
time were associated with those objects.

In describing the hostile meeting between Satan and Death before the
Gates of Hell, he writes:

                            On the other side,
    Incensed with indignation, Satan stood
    Unterrified, and like a comet burned,
    That fires the length of Ophiuchus huge
    In the arctic sky, and from his horrid hair
    Shakes pestilence and war.--ii. 706-11.

This passage is eminently descriptive of the appearance of a great
comet, and the occasion on which it is introduced adds to the intensity
of the lurid imaginings and feelings of terror and dismay with which
these objects have always been regarded. The comparison of the enraged
Prince of Hell with one of those mysterious and fiery looking visitors
to our skies was a grand conception of the poet's, and one worthy of the
mighty combatant. Ophiuchus (the Serpent-bearer) is a large
constellation which occupies a rather barren region of the heavens to
the south of Hercules. It has a length of about forty degrees, and is
represented by the figure of a man bearing a serpent in both hands. It
is not easy to imagine why Milton should have assigned the comet to
this uninteresting constellation; he may possibly have seen one in this
part of the sky, or his poetical ear may have perceived that the
expression 'Ophiuchus huge,' which has about it a ponderous rhythm, was
well adapted for the poetic description of a comet.

The only other allusion in the poem to a comet is near its conclusion,
when the Cherubim descend to take possession of the Garden, prior to the
removal of Adam and Eve--

                              High in front advanced,
    The brandished sword of God before them blazed,
    Fierce as a comet; which with torrid heat,
    And vapour as the Lybian air adust
    Began to parch that temperate clime.--xii. 632-36.


FALLING STARS

On any clear night an observer can, by attentively watching the heavens,
perceive a few of those objects which become visible for a moment as a
streak of light and then vanish. They are the result of the combustion
of small meteoric masses having a celestial origin, and travelling with
cosmical velocity, and which, in their headlong flight, become so heated
by contact with the Earth's atmosphere that they are converted into
glowing vapour. This vapour when it cools condenses into fine powder or
dust, and gradually descends upon the Earth's surface, where it can be
detected.

Shooting stars become visible at a height varying between twenty and one
hundred and thirty miles, and their average velocity has been estimated
at about thirty miles a second. Though casual falling stars can be seen
at all times in every part of the heavens, yet there are certain periods
at which they appear in large numbers, and have been observed to radiate
from certain well-defined parts of the sky. When the radiant point is
overhead, the falling stars spread out and resemble a parachute of fire;
but when it is below the horizon, the stars ascend upwards like rockets
into the sky. The radiant point is fixed among the stars, so that at the
commencement of a shower it may be overhead, and before the termination
of the display it may have travelled below the horizon. The radiant is
usually named after the constellation in which it is observed.

The November meteors are called Leonids, because they radiate from a
point in the constellation Leo; those in Taurus are called Taurids; in
Perseus, Perseids; in Lyra, Lyraïds; and in Andromeda, Andromedes,
because their radiant points are situated in those constellations.

The falling stars that have attracted most attention are those which
appear on or about November 13. Every year at this period they can be
seen in greater or less numbers, and on referring to numerous past
records it has been ascertained that a magnificent display of those
objects occurs every thirty-three years. The earliest historical
allusion to this meteoric shower is by Theophanes, who wrote that in the
year 472 A.D. the sky at Constantinople appeared to be on fire with
falling stars. In the year 902 A.D. another remarkable display took
place, and from that time until 1833 twelve conspicuous displays are
recorded as having occurred at recurring intervals of thirty-three
years. The grandest display of this kind that was ever witnessed
occurred in 1833. It was visible over nearly the whole of the American
continent, and, having commenced at midnight, lasted for four or five
hours. The falling stars were so numerous that they appeared to rain
upon the Earth, and caused the utmost consternation and terror among
those who witnessed the phenomenon, many persons having imagined that
the end of the world was at hand. The regular recurrence of these
meteoric displays has been satisfactorily explained by the assumption
that round the Sun there travels in an elliptical orbit with planetary
velocity a vast shoal of meteoric bodies some millions of miles in
length and several hundred thousand miles in breadth. The nearest point
of their orbit to the Sun coincides with the Earth's orbit, and the most
distant part extends beyond the orbit of Uranus. These bodies accomplish
a circuit of their orbit in 33-1/4 years. The Earth in her annual
revolution intersects the path of the meteors, and when this occurs some
falling stars can always be seen; but when the intersection happens at
the time the shoal is passing, then there results a grand meteoric
display. Numerous other meteoric swarms travel in orbital paths round
the Sun.

Milton, in his poem, alludes to falling stars upon two occasions. In
describing the fall of Mulciber from Heaven he says:--

                                      from morn
    To noon he fell, from noon to dewy eve,
    A summer's day; and with the setting sun
    Dropt from the zenith like a falling star,
    On Lemnos the Ægaean isle.--i. 742-46.

The rapid flight of the archangel Uriel from the Sun to the Earth is
described in the following lines:--

    Thither came Uriel, gliding through the even
    On a sunbeam, swift as a shooting star
    In autumn thwarts the night, when vapours fired
    Impress the air, and shows the mariner
    From what point of his compass to beware
    Impetuous winds.--iv. 555-60.

Milton mentions the season of the year in which those stars are most
frequently seen, and refers to an ancient belief by which they were
regarded as the precursors of stormy weather. A translation from Virgil
contains a similar allusion to them--

    Oft shalt thou see ere brooding storms arise,
    Star after star glide headlong down the skies.

The standard borne by the Cherub Azazel is described as having--

    Shone like a meteor streaming to the wind.--i. 537.




CHAPTER IX

MILTON'S IMAGINATIVE AND DESCRIPTIVE ASTRONOMY


The theme chosen by Milton for his great epic, viz. the Fall of Man and
his expulsion from Paradise--perhaps the most momentous incident in the
history of the human race--was one worthy of the genius of a great poet
and in the treatment of which Milton has been sublimely successful. The
newly created Earth; the untainted loveliness of the Paradise in which
our first parents dwelt during their innocence; their temptation; their
fall and removal from the happy garden, furnished a theme which afforded
him an opportunity for the display of his unrivalled poetic genius.

Though the chief interest in the poem is centred in the Garden of Eden
and its occupants, yet Milton was enabled, by the comprehensive manner
in which he treated his subject, to introduce into his work a cosmology
which embraced not only the system to which our globe belongs, but the
entire starry heavens by which we are surrounded. But the universality
of his genius did not rest here. In the utterance of his sacred song he
soared beyond the starry sphere, describing himself as wrapt above the
pole--the starry pole--up to the Empyrean, or Heaven of Heavens, the
ineffable abode of the Deity and the blissful habitation of angelic
beings who, in adoration and worship, surround the throne of the Most
High.

Descending to that nether world at the opposite pole of the universe, in
the lowest depth of Chaos, the place prepared by Eternal Justice for the
rebellious, he unfolds to our horror-stricken gaze the terrors of this
infernal region; its fiery deluge of ever-burning sulphur; its 'regions
of sorrow;' its 'doleful shades'--the unhappy abode of fallen angels who
'in floods and whirlwinds of tempestuous fire,' alternated by exposure
to unendurable cold and icy torment, experience the direful consequences
of their apostacy.

Milton's 'Paradise Lost' may be regarded as the loftiest intellectual
effort in the whole range of literature. In it we find all that was
known of science, philosophy, and theology. The theme, founded upon a
Bible narrative, itself written under divine inspiration, embraces the
entire system of Christian doctrine as revealed in the Scriptures, and
many of the noblest passages in the sacred volume are introduced into
the poem expressed in the lofty utterance of flowing and harmonious
verse. The choicest classical writings of Greek and Latin authors; the
mythological and traditional beliefs of ancient nations; historical
incidents of valour and renown and all that was great and good in the
annals of mankind were laid under contribution by Milton in the
illustration and embellishment of his poem.

In order to obtain a basis or foundation upon which to construct his
great epic, Milton found it necessary to localise the regions of space
in which the principal events mentioned in his poem are described as
having occurred. The unfathomable abyss of space may be regarded as an
uncircumscribed sphere boundless on all sides round, and so far as we
can comprehend of infinite extent. This sphere Milton divided into two
hemispheres--an upper and a lower. The upper was called Heaven, or the
Empyrean--a glorified region of boundless dimensions; the lower
hemisphere embraced Chaos--a dark, fathomless abyss in which the
elements of matter existed in a state of perpetual tumult and wild
uproar. The occurrence of a rebellion in Heaven necessitated a further
division of the sphere. The revolt, headed by Lucifer, one of the
highest archangels, afterwards known as Satan, who drew after him a
third of the angelic host, contested the supremacy of Heaven with
Michael and the angels which kept their loyalty. After two days'
battle--

                        Him the Almighty Power
    Hurled headlong flaming from the ethereal sky,
    With hideous ruin and combustion, down
    To bottomless perdition; there to dwell
    In adamantine chains and penal fire.--i. 44-48.

Having been precipitated over the crystal wall of Heaven into the deep
abyss, Milton says:--

    Nine days they fell; confounded Chaos roared,
    And felt tenfold confusion in their fall
    Through his wild Anarchy; so huge a rout
    Encumbered him with ruin. Hell at last,
    Yawning, received them whole, and on them closed.--vi. 871-75.

Hell, Milton locates in the lowest depth of Chaos, a region cut off from
the body of Chaos, through which the expelled angels fell for nine days
before reaching their destined habitation. There are now three divisions
of space: HEAVEN, CHAOS, and HELL. But a fourth is required to enable
Milton to complete his scheme for the delineation of his poem. The Earth
and starry universe were not as yet called into existence, but after the
overthrow of the rebellious angels, God, by circumscribing a portion of
Chaos situated immediately underneath the Empyrean, created the Mundane
Universe, or the 'Heavens and the Earth.'[15] This new universe He
reclaimed from Chaos, and with the embryo elements of matter--

    His dark materials to create new worlds.--ii. 916.

He formed the Earth and all the countless shining orbs visible overhead,
and the myriads more which the telescope reveals, scattered in
apparently endless profusion over the circular immensity of space. It is
this new universe--the Earth and Starry Heavens--that claims our chief
attention, and in the delineation of Milton's imaginative and
descriptive powers it is to this latest manifestation of Divine wisdom
and might that our remarks shall principally apply. After the expulsion
of the rebel angels from Heaven, God sent His Son, the Messiah to create
the new universe--a work of omnipotence described by Milton in a manner
worthy of so magnificent a display of almighty power--

                                Meanwhile the Son
    On his great expedition now appeared,
    Girt with omnipotence, with radiance crowned
    Of majesty divine: sapience and love
    Immense; and all his Father in Him shone.
    About his chariot numberless were poured
    Cherub and Seraph, Potentates and Thrones,
    And Virtues, winged Spirits, and chariots winged
    From the armoury of God, where stand of old
    Myriads, between two brazen mountains lodged
    Against a solemn day, harnessed at hand,
    Celestial equipage; and now came forth
    Spontaneous, for within them Spirit lived,
    Attendant on their Lord. Heaven opened wide
    Her ever-during gates, harmonious sound!
    On golden hinges moving, to let forth
    The King of Glory, in his powerful Word
    And Spirit, coming to create new worlds.
    On Heavenly ground they stood, and from the shore
    They viewed the vast immeasurable abyss
    Outrageous as a sea, dark, wasteful, wild,
    Up from the bottom turned by furious winds
    And surging waves, as mountains to assault
    Heaven's highth, and with the centre mix the pole.
    'Silence, ye troubled Waves, and thou Deep, peace!'
    Said then the omnific Word: 'your discord end!'
    Nor stayed; but on the wings of Cherubim
    Uplifted, in paternal glory rode
    Far into Chaos, and the World unborn;
    For Chaos heard his voice. Him all his train
    Followed in bright procession, to behold
    Creation, and the wonders of his might.
    Then stayed the fervid wheels, and in his hand
    He took the golden compasses, prepared
    In God's eternal store, to circumscribe
    This Universe, and all created things.
    One foot he centred, and the other turned
    Round through the vast profundity obscure;
    And said, 'Thus far extend, thus far thy bounds;
    This be thy just circumference, O World!'
    Thus God the Heaven created, thus the Earth,
    Matter unformed and void. Darkness profound
    Covered the abyss; but on the watery calm
    His brooding wings the Spirit of God outspread,
    And vital virtue infused, and vital warmth,
    Throughout the fluid mass; but downward purged
    The black, tartareous, cold, infernal dregs,
    Adverse to life; then founded, then conglobed
    Like things to like; the rest to several place
    Disparted, and between spun out the Air;
    And Earth self balanced on her centre hung.--vii. 192-242.

Milton begins his narrative of the Creation by describing the progress
of the Deity on His great expedition, accompanied by hosts of angels and
surrounded with all the solemn pomp and splendour of Heaven. The
brilliant throng having passed through Heaven's gates, which opened wide
their portals, they beheld in front of them the dark abyss of Chaos--a
tempest-tossed sea of warring elements upturned in wild confusion. At
God's instant command silence and peace reigned over the deep, and
tranquil calm succeeded noisy discord. Then on the wings of Cherubim He
rode far into Chaos, and with His golden compasses decreed the
dimensions of the universe by circumscribing the vast vacuity of space.
Into the elements which hasted to their several places, His Spirit
infused vital warmth and caused the formless mass of matter to assume
the figure of a sphere, and thus the Earth poised on her axis
unsupported, and in darkness shrouded hung suspended in space. The
placing of the golden compasses in the hands of the Creator, with which
He measured out the heavens, is a noble conception on the part of
Milton, and one most appropriate, since the construction of the universe
is based upon the principles of geometrical science.

    'Let there be Light!' said God; and forthwith Light
    Ethereal, first of things, quintessence pure,
    Sprung from the Deep; and from her native east
    To journey through the aëry gloom began,
    Sphered in a radiant cloud; for yet the Sun
    Was not; she in a cloudy tabernacle
    Sojourned the while. God saw the light was good;
    And light from darkness by the hemisphere
    Divided; light the day, and darkness night
    He named. Thus was the first day even and morn:
    Nor passed uncelebrated, nor unsung
    By the celestial quires, when orient light
    Exhaling first from darkness they beheld;
    Birthday of Heaven and Earth; with joy and shout
    The hollow universal orb they filled,
    And touched their golden harps, and hymning praised
    God and his works: Creator Him they sung,
    Both when first evening was, and when first morn.--vii. 243-60.

The appearance of Light, which sprung into existence at the fiat of the
Creator, was the next great event witnessed by beholding
angels--birthday of Heaven and Earth, first morning and first evening,
which the celestial choirs celebrated with praise and shouts of joy.
The creation of the firmament was the great work of the second day.

    Again God said, 'Let there be firmament
    Amid the waters, and let it divide
    The waters from the waters!' And God made
    The firmament, expanse of liquid, pure,
    Transparent, elemental air, diffused
    In circuit to the uttermost convex
    Of this great round--partition firm and sure,
    The waters underneath from those above
    Dividing; for as the Earth, so He the World
    Built on circumfluous waters calm, in wide
    Crystalline ocean, and the loud misrule
    Of Chaos far removed, lest fierce extremes
    Contiguous might distemper the whole frame:
    And Heaven he named the Firmament. So even
    And morning chorus sung the second day.--vii. 261-275.

After describing the gathering of the waters off the face of the globe
into seas, causing the dry land to appear, which at the word of God
became clothed with vegetation, rendering the Earth a habitable abode,
Milton proceeds to describe the creation of the heavenly bodies--

    Again the Almighty spake: 'Let there be Lights
    High in the expanse of Heaven, to divide
    The day from night; and let them be for signs,
    For seasons, and for days, and circling years;
    And let them be for lights, as I ordain
    Their office in the firmament of Heaven,
    To give light on the Earth!' and it was so.
    And God made two great Lights, great for their use
    To Man, the greater to have rule by day,
    The less by night, altern; and made the Stars,
    And set them in the firmament of Heaven
    To illuminate the Earth, and rule the day
    In their vicissitude, and rule the night,
    And light from darkness to divide. God saw,
    Surveying his great work, that it was good:
    For, of celestial bodies, first, the Sun,
    A mighty sphere He framed, unlightsome first,
    Though of ethereal mould; then formed the Moon
    Globose, and every magnitude of Stars,
    And sowed with stars the Heaven thick as a field.
    Of light by far the greater part he took,
    Transplanted from her cloudy shrine, and placed
    In the Sun's orb, made porous to receive
    And drink the liquid light; firm to retain
    Her gathered beams, great palace now of Light.
    Hither, as to their fountain, other stars
    Repairing, in their golden urns draw light,
    And hence the morning planet gilds her horns;
    By tincture or reflection they augment
    Their small peculiar, though, from human sight
    So far remote, with diminution seen.
    First in his east the glorious lamp was seen,
    Regent of day, and all the horizon round
    Invested with bright rays, jocund to run
    His longitude through Heaven's high road; the grey
    Dawn, and the Pleiades before him danced,
    Shedding sweet influence. Less bright the Moon,
    But opposite in levelled west was set
    His mirror, with full face borrowing her light
    From him; for other light she needed none
    In that aspect, and still that distance keeps
    Till night; then in the east her turn she shines,
    Revolved on Heaven's great axle, and her reign
    With thousand lesser lights dividual holds,
    With thousand thousand stars that then appeared
    Spangling the hemisphere. Then first adorned
    With their bright luminaries, that set and rose,
    Glad evening and glad morn crowned the fourth day.--vii. 339-86.

The first creation was Light, and Milton, according to Scriptural
testimony, ascribes its origin to the bidding of the Creator. 'God said,
Let there be light; and there was light!' The Sun he describes as a
mighty sphere, but at first non-luminous. There was light, but no sun.
The reason usually given in explanation of this phenomenon is, that the
heavenly bodies were created at the same time as the Earth, but were
rendered invisible by a canopy of vapour and cloud which enveloped the
newly-formed globe; and that afterwards, when it dispersed, they
appeared in the firmament, shining in all their pristine splendour.
Milton does not, however, adhere to this view of things, but says that
light for the first three days sojourned in a cloudy shrine or
tabernacle, and was afterwards transplanted in the Sun, which became a
great palace of light.

He expresses himself in a somewhat similar manner in Book III., which
opens with an address to Light--one of the most beautiful passages in
the poem, in which he alludes to his blindness when expressing his
thoughts and sentiments with regard to this ethereal medium, which
conveys to us the pleasurable sensation of vision--

    Hail, holy Light! offspring of Heaven first-born!
    Or of the Eternal co-eternal beam,
    May I express thee unblamed? since God is light,
    And never but in unapproached light
    Dwelt from eternity--dwelt then in thee,
    Bright effluence of bright essence increate!
    Or hear'st thou rather, pure Ethereal stream,
    Whose fountain who shall tell? Before the Sun,
    Before the Heavens thou wert, and at the voice
    Of God, as with a mantle, didst invest
    The rising world of waters dark and deep,
    Won from the void and formless Infinite.--iii. 1-12.

The Sun having become a lucent orb, Milton poetically describes how the
planets repair to him as to a fountain, and in their golden urns draw
light; and how the morning planet Venus gilds her horns illumined by his
rays. The poet associates joyous ideas with the new-born universe. The
Sun, now the glorious regent of day, begins his journey in the east,
lighting up the horizon with his beams; whilst before him danced the
grey dawn, and the Pleiades shedding sweet influences. There existed an
ancient belief that the Earth was created in the spring, and in April
the Sun is in the zodiacal constellation Taurus, in which are also
situated the Pleiades; they rise a little before the orb, and precede
him in his path through the heavens. The stars of this group have always
been regarded with a peculiar sacredness, and their rays, mingling with
those of the Sun, were believed to shed sweet influences upon the Earth.
The Moon, less bright, with borrowed light, in her turn shines in the
east, and, with the thousand thousand luminaries that spangle the
firmament, reigns over the night.

We learn in Book III. that the archangel Uriel, who was beguiled by
Satan, witnessed the Creation, and described how the heavenly bodies
were brought into existence, he having perceived what we should call the
gaseous elements of matter rolled into whorls and vortices which became
condensed into suns and systems of worlds. This mighty angel says:--

    I saw when, at his word the formless mass,
    This World's material mould, came to a heap:
    Confusion heard his voice, and wild Uproar
    Stood ruled, stood vast Infinitude confined;
    Till at his second bidding darkness fled,
    Light shone, and order from disorder sprung.
    Swift to their several quarters hasted then
    The cumbrous elements, Earth, Flood, Air, Fire;
    And this ethereal quintessence of Heaven
    Flew upward, spirited with various forms,
    That rolled orbicular, and turned to stars
    Numberless, as thou seest, and how they move;
    Each had his place appointed, each his course;
    The rest in circuit walls this Universe.--iii. 708-21.

In his sublime description of the Creation Milton has adhered with
marked fidelity to the Mosaic version, as narrated in the first two
chapters of Genesis, when God, by specific acts in certain stated
periods of time, created the visible universe and all that it contains.

The successive acts of creation are described in words almost identical
with those of Scripture, embellished and adorned with all the wealth of
expression which our language is capable of affording. The several
scenes presented to the imagination, and witnessed by hosts of admiring
angels as each portion of the magnificent work was accomplished, are
full of a grandeur and majesty worthy of the loftiest conceivable effort
of Divine power and might.

The return of the Creator after the completion of His great work is
described by Milton in a manner worthy of the progress of Deity through
the celestial regions. The whole creation rang with jubilant delight,
and the bright throng which witnessed the wonders of His might followed
Him with acclamation, ascending by the glorified path of the Milky Way
up to His high abode--the Heaven of Heavens--

    Here finished He, and all that He had made
    Viewed, and behold! all was entirely good.
    So even and morn accomplished the sixth day:
    Yet not till the Creator from his work
    Desisting, though unwearied, up returned,
    Up to the Heaven of Heavens, His high abode,
    Thence to behold this new created World,
    The addition of his empire, how it showed
    In prospect from His throne, how good, how fair,
    Answering his great idea. Up He rode,
    Followed with acclamation, and the sound
    Symphonious of ten thousand harps, that tuned
    Angelic harmonies: The Earth, the Air
    Resounded (thou remember'st, for thou heard'st)
    The Heavens and all the constellations rung,
    The planets in their stations listening stood,
    While the bright pomp ascended jubilant.
    'Open ye everlasting gates!' they sung;
    'Open ye Heavens! your living doors; let in
    The great Creator, from his work returned
    Magnificent, his six days' work, a World;
    Open, and henceforth oft; for God will deign
    To visit oft the dwellings of just men,
    Delighted; and with frequent intercourse
    Thither will send his winged messengers
    On errands of supernal grace.' So sung
    The glorious train ascending: He through Heaven,
    That opened wide her blazing portals, led
    To God's eternal house direct the way--
    A broad and ample road, whose dust is gold,
    And pavement stars, as stars to thee appear
    Seen in the Galaxy, that Milky Way
    Which nightly as a circling zone thou seest
    Powdered with stars.--vii. 548-81.

Milton, throughout his description of the Creation, sustains with lofty
eloquence his sublime conception of this latest display of almighty
power; and invests with becoming majesty all the acts of the Creator,
who, when He finished His great work, saw that all was entirely good.

Shortly after the creation of the new universe, Satan, having escaped
from Hell, plunged into the abyss of Chaos, and, after a long and
arduous journey upwards, in which he had to fight his way through the
surging elements that raged around him like a tempestuous sea, he
reached the upper confines of this region where less confusion
prevailed, and where a glimmering dawn of light penetrated its darkness
and gloom, indicating that the limit of the empire of Chaos and ancient
Night had been reached by the adventurous fiend. Pursuing his way with
greater ease, he leisurely beholds the sight which is opening to his
eyes--a sight rendered more glorious by his long sojourn in darkness. He
sees:--

    Far off the empyreal Heaven, extended wide
    In circuit, undetermined square or round,
    With opal towers and battlements adorned
    Of living sapphire, once his native seat,
    And, fast by, hanging in a golden chain,
    This pendent World, in bigness as a star
    Of smallest magnitude close by the Moon.--ii. 1047-53.

He gazes upon his native Heaven where once he dwelt, and observes the
pendent world in quest of which he journeyed hither--hung by a golden
chain from the Empyrean and no larger than a star of the smallest
magnitude when close by the Moon. In this passage Milton does not allude
to the Earth, which was invisible, but to the entire starry heavens--the
newly created universe reclaimed from Chaos, which, when contrasted with
the Empyrean, appeared in size no larger than the minutest star when
compared with the full moon. Pursuing his journey, the new universe as
it is approached expands into a globe of vast dimensions; its convex
surface--round which the chaotic elements in stormy aspect
lowered--seemed a boundless continent, dark, desolate, and starless,
except on the side next to the wall of Heaven, which though far-distant
afforded it some illumination by its reflected light. Satan, having
alighted on this convex shell which enclosed the universe, wandered long
over its bleak and dismal surface, until his attention was attracted by
a gleam of light which appeared through an opening at its zenith right
underneath the Empyrean. Thither he directed his steps, and perceived a
structure resembling a staircase, or ladder, which formed the only means
of communication between Heaven and the new creation, and upon which
angels descended and ascended--

                        Far distant he descries,
    Ascending by degrees magnificent
    Up to the wall of Heaven, a structure high;
    At top whereof, but far more rich, appeared
    The work as of a kingly palace gate,
    With frontispiece of diamond and gold
    Embellished; thick with sparkling orient gems
    The portal shone, inimitable on Earth
    By model, or by shading pencil drawn.
    The stairs were such as whereon Jacob saw
    Angels ascending and descending, bands
    Of Guardians bright, when he from Esau fled
    To Padan Aram, in the field of Luz
    Dreaming by night under the open sky,
    And waking cried, '_This is the gate of Heaven._'--iii. 501-15.

Sometimes this mysterious structure was drawn up to Heaven and
invisible. At the time that Satan reached the opening, the stairs were
lowered, and standing at their base he looked down with wonder upon the
entire starry universe--

    Such wonder seized, though after Heaven seen,
    The Spirit malign, but much more envy seized,
    At sight of all this World beheld so fair,
    Round he surveys (and well might, where he stood
    So high above the circling canopy
    Of night's extended shade) from eastern point
    Of Libra to the fleecy star that bears
    Andromeda far off Atlantic seas
    Beyond the horizon; then from pole to pole
    He views in breadth, and without longer pause,
    Down right into the World's first region throws
    His flight precipitant, and winds with ease
    Through the pure marble air his oblique way
    Amongst innumerable stars, that shone
    Stars distant, but nigh hand seemed other worlds,
    Or other worlds they seemed, or happy isles,
    Like those Hesperian Gardens famed of old,
    Fortunate fields, and groves, and flowery vales;
    Thrice happy isles! But who dwelt happy there
    He staid not to inquire: above them all
    The golden Sun, in splendour likest Heaven
    Allured his eye: thither his course he bends
    Through the calm firmament, (but up or down
    By centre or eccentric hard to tell
    Or longitude) where the great luminary,
    Aloof the vulgar constellations thick,
    That from his lordly eye keep distance due,
    Dispenses light from far. They, as they move
    Their starry dance in numbers that compute
    Days, months, and years, towards his all-cheering lamp
    Turn swift their various motions, or are turned
    By his magnetic beam, that gently warms
    The Universe, and to each inward part
    With gentle penetration, though unseen,
    Shoots invisible virtue even to the Deep;
    So wondrously was set his station bright.--iii. 552-87.

The Ptolemaic cosmology having been adopted by Milton in the elaboration
of his poem, he describes the universe in conformity with the doctrines
associated with this form of astronomical belief. To each of the first
seven spheres which revolved round the steadfast Earth there was
attached a heavenly body; the eighth sphere embraced all the fixed
stars, a countless multitude; the ninth the crystalline; and enclosing
all the other spheres as if in a shell was the tenth sphere, or Primum
Mobile, which in its diurnal revolution carried round with it all the
other spheres. The nine inner spheres were transparent, but the tenth
was an opaque solid shell-like structure, which enclosed the new
universe and constituted the boundary between it and Chaos underneath
and the Empyrean above. It was on the surface of this sphere that Satan
wandered until he discovered the opening at its zenith, where, by means
of a staircase or ladder, communication was maintained with the
Empyrean. Standing on the lower steps of this structure he paused for a
moment to look down into the glorious universe which lay beneath him--

                                  another Heaven
    From Heaven-gate not far, founded in view
    On the clear hyaline the glassy sea.--vii. 617-19.

He beholds it in all its dimensions, from pole to pole, and
longitudinally from Libra to Aries, then without hesitation precipitates
himself down into the world's first region, and winds his way with ease
among the fixed stars. Around him he sees innumerable shining worlds,
sparkling and glittering in endless profusion over the circumscribed
immensity of space--mighty constellations that shone from afar;
clustering aggregations of stars; floating islands of light; twinkling
systems rising out of depths still more profound, and a zone luminous
with the light of myriads of lucid orbs verging on the confines of the
universe. All these worlds the fiend passed unheeded, nor stayed he to
inquire who dwelt happy there. In splendour above them all the Sun
attracted his attention and, directing his course towards the great
luminary of our system, he alights on the surface of the orb.

Milton now makes a digression in order to describe what Satan observed
in the Sun after having landed there. The poet embraces an opportunity
for exercising his imaginative and descriptive powers by giving an ideal
description of what, judging from the appearance of the orb, might be
the natural condition of things existing on his surface--

    There lands the Fiend, a spot like which perhaps
    Astronomer in the Sun's lucent orb
    Through his glazed optic tube, yet never saw.
    The place he found beyond expression bright,
    Compared with aught on Earth, metal or stone;
    Not all parts like, but all alike informed
    With radiant light, as glowing iron with fire;
    If metal, part seemed gold, part silver clear;
    If stone, carbuncle most or chrysolite,
    Ruby or topaz, to the twelve that shone
    In Aaron's breastplate, and a stone besides,
    Imagined rather oft than elsewhere seen;
    That stone, or like to that, which here below
    Philosophers in vain so long have sought,
    In vain, though by their powerful art they bind
    Volatile Hermes, and call up unbound
    In various shapes old Proteus from the sea,
    Drained through a limbec to his native form.
    What wonder then if fields and regions here
    Breathe forth elixir pure, and rivers run
    Potable gold, when, with one virtuous touch,
    The arch-chemic Sun, so far from us remote,
    Produces, with terrestrial humour mixed,
    Here in the dark so many precious things
    Of colour glorious, and effect so rare?
    Here matter new to gaze the Devil met
    Undazzled; far and wide his eye commands;
    For sight no obstacle found here, nor shade,
    But all sunshine, as when his beams at noon
    Culminate from the equator, as they now
    Shot upward still direct, whence no way round
    Shadow from body opaque can fall; and the air,
    Nowhere so clear sharpened his visual ray
    To objects distant far, whereby he soon
    Saw within here a glorious Angel stand.--iii. 588-622.

The physical structure of the interior of the Sun is unknown; all that
we see of the orb is the photosphere--the dazzling luminous envelope
which indicates to the eye the boundary of the solar disc, and which is
the source of light and heat. Milton, in his imaginative and beautifully
poetical description of the Sun, is not more fanciful in his conception
of the nature of the refulgent orb than a renowned astronomer (Sir
William Herschel) who writes in the following strain: 'A cool, dark,
solid globe, its surface diversified with mountains and valleys, clothed
in luxuriant vegetation and richly stored with inhabitants, protected by
a heavy cloud-canopy from the intolerable glare of the upper luminous
region, where the dazzling coruscations of a solar aurora some thousands
of miles in depth evolved the stores of light and heat which vivify our
world.' Satan, disguised as a cherub, makes himself known to Uriel,
Regent of the Sun. The upright Seraph in response to his request directs
him to the Earth, the abode of Man--

    Look downward on that Globe, whose hither side
    With light from hence, though but reflected, shines,
    That place is Earth, the seat of Man; that light
    His day, which else, as the other hemisphere,
    Night would invade; but there neighbouring Moon
    (So call that opposite fair star) her aid
    Timely interposes, and her monthly round
    Still ending, still renewing, through mid-Heaven,
    With borrowed light her countenance triform
    Hence fills and empties, to enlighten the Earth,
    And in her pale dominion checks the night.--iii. 722-32.

It would be impossible not to feel impressed with the accuracy and
comprehensiveness of Milton's astronomical knowledge; and how he has
united in charming poetic expression the dry details of science with the
divine inspiration of the heavenly muse. The distinctive appearances of
the Sun, Moon, planets, and stars; their functional importance as
regards this terrestrial sphere; the splendour and lustre peculiar to
each; and the glory displayed in the entire created heavens, are
portrayed with a skill indicative of a masterly knowledge of the science
of astronomy.

    Descend from Heaven, Urania, by that name
    If rightly thou art called, whose voice divine
    Following, above the Olympian hill I soar,
    Above the flight of Pegasean wing!
    The meaning, not the name, I call; for thou
    Nor of the Muses nine, nor on the top
    Of old Olympus dwell'st; but heavenly-born,
    Before the hills appeared or fountain flowed,
    Thou with Eternal Wisdom didst converse,
    Wisdom thy sister, and with her didst play
    In presence of the Almighty Father, pleased
    With thy celestial song. Up led by thee,
    Into the Heaven of Heavens I have presumed,
    An earthly guest, and drawn empyreal air,
    Thy tempering. With like safety guided down,
    Return me to my native element;
    Lest, from this flying steed unreined, (as once
    Belerophon, though from a lower clime)
    Dismounted, on the Aleian field I fall,
    Erroneous there to wander, and forlorn.
    Half yet remains unsung, but narrower bound
    Within the visible diurnal sphere.
    Standing on Earth, not rapt above the pole,
    More safe I sing with mortal voice, unchanged
    To hoarse or mute, though fallen on evil days,
    On evil days though fallen, and evil tongues,
    In darkness, and with dangers compassed round,
    And solitude; yet not alone, while thou
    Visit'st my slumbers nightly, or when morn
    Purples the east. Still govern thou my song,
    Urania, and fit audience find though few.--vii. 1-32.

The Muses were Greek mythological divinities who possessed the power of
inspiring song, and were the patrons of poets and musicians. According
to Hesiod they were nine in number and presided over the arts. Urania
was the Goddess of Astronomy, and Calliope the Goddess of Epic Poetry.
They are described as the daughters of Zeus, and Homer alludes to them
as the goddesses of song who dwelt on the summit of Mount Olympus. They
were the companions of Apollo, and accompanied with song his playing on
the lyre at the banquets of the Immortals. Milton does not invoke the
mythological goddess, but Urania the Heavenly Muse, whose aid he also
implores at the commencement of his poem prior to his flight above the
Aonian Mount. Under her divine guidance he ascended to the Heaven of
Heavens and breathed empyreal air, her tempering; in like manner he
requests her to lead him down to his native element lest he should meet
with a fate similar to what befell Bellerophon. Half his task he has
completed, the other half, confined to narrower bounds within the
visible diurnal sphere, remains unsung, and in its fulfilment he still
implores his celestial patroness to govern his song.

The natural phenomena which occur as a consequence of the motions of the
heavenly bodies and the diurnal rotation of the Earth on her axis, are
accompanied by agreeable alternations in the aspect of nature with which
every one is familiar. The rosy footsteps of morn; the solar splendour
of noonday; the fading hues of even; and night with her jewelled courts
and streams of molten stars, have been sung with rapturous admiration by
poets of every nation and in every age. They, as ardent lovers of
nature, have described in choicest language the pleasing vicissitudes
brought about by the real and apparent motions of the celestial orbs.

In this respect Milton is unsurpassed by any poet in ancient or in
modern times. The occasions on which he describes the heavenly bodies,
or alludes to them in association with other phenomena, testify to the
felicity of his thoughts and to the greatness of his poetic genius.
Surely no poet has ever given us a lovelier description of evening, or
has added more to its exquisite beauty by his allusion to the celestial
orbs, than Milton when he describes the first evening in Paradise--

    Now came still Evening on, and Twilight gray
    Had in her sober livery all things clad;
    Silence accompanied; for beast and bird,
    They to their grassy couch, these to their nests
    Were slunk, all but the wakeful nightingale.
    She all night long her amorous descant sung;
    Silence was pleased. Now glowed the firmament
    With living sapphires: Hesperus that led
    The starry host, rode brightest, till the Moon,
    Rising in clouded majesty, at length
    Apparent queen, unveiled her peerless light,
    And o'er the dark her silver mantle threw.--iv. 598-609.

In the avowal of her conjugal love, Eve, with charming expression,
associates the orbs of the firmament with the delightful appearances of
nature which presented themselves to her observation after she awoke to
the consciousness of intelligent existence.

    Sweet is the breath of Morn, her rising sweet,
    With charm of earliest birds: pleasant the Sun,
    When first on this delightful land he spreads
    His orient beams, on herb, tree, fruit, and flower,
    Glistering with dew; fragrant the fertile Earth
    After soft showers; and sweet the coming on
    Of grateful Evening mild; then silent Night,
    With this her solemn bird, and this fair Moon,
    And these the gems of Heaven, her starry train:
    But neither breath of Morn, when she ascends
    With charm of earliest birds; nor rising Sun
    On this delightful land; nor herb, fruit, flower,
    Glistering with dew; nor fragrance after showers;
    Nor grateful Evening mild; nor silent Night,
    With this her solemn bird; nor walk by Moon,
    Or glittering star-light, without thee is sweet.
    But wherefore all night long shine these? for whom
    This glorious sight, when sleep hath shut all eyes?--iv. 641-58.

One of the charms of Milton's verse is the devoutly poetical sentiment
which pervades it. His thoughts, though serious, are not austere or
gloomy, and it is in his loftiest musings that his reverence becomes
most apparent. This feeling is conspicuous in Adam's reply to the
inquiry addressed to him by Eve--

    Daughter of God and Man, accomplished Eve,
    These have their course to finish round the Earth
    By morrow evening, and from land to land
    In order, though to nations yet unborn,
    Ministering light prepared, they set and rise;
    Lest total Darkness should by night regain
    Her old possession, and extinguish life
    In Nature and all things; which these soft fires
    Not only enlighten, but with kindly heat
    Of various influence foment and warm,
    Temper or nourish, or in part shed down
    Their stellar virtue on all kinds that grow
    On Earth, made hereby apter to receive
    Perfection from the Sun's more potent ray.
    These, then, though unbeheld in deep of night,
    Shine not in vain; nor think, though men were none,
    That Heaven would want spectators, God want praise:
    Millions of spiritual creatures walk the Earth
    Unseen, both when we wake, and when we sleep:
    All these with ceaseless praise his works behold
    Both day and night. How often from the steep
    Of echoing hill or thicket, have we heard
    Celestial voices to the midnight air,
    Sole, or responsive each to other's note
    Singing their Great Creator! Oft in bands
    While they keep watch, or nightly rounding walk,
    With heavenly touch of instrumental sounds
    In full harmonic number joined, their songs
    Divide the night, and lift our thoughts to Heaven.--iv. 660-88.

The Morning Hymn of Praise which Adam and Eve offer up in concert to
their Maker contains their loftiest thoughts and most reverent
sentiments, expressed in melodiously flowing verse. In their solemn
invocations they call upon the orbs of the firmament to join in
praising and extolling the Creator, and in their devout enthusiasm and
adoration address by name those that are most conspicuous. Hesperus,
'fairest of stars,' is asked to praise Him in her sphere. The Sun, great
image of his Maker, is told to acknowledge Him his greater, and to sound
His praise in his eternal course. The Moon, the fixed stars, and the
planets are called upon to resound the praise of the Creator, whose
glory is declared in the Heavens--

    Fairest of Stars, last in the train of night,
    If better thou belong not to the dawn,
    Sure pledge of day, that crown'st the smiling morn
    With thy bright circlet, praise Him in thy sphere
    While day arises, that sweet hour of prime.
    Thou Sun, of this great world both eye and soul,
    Acknowledge Him thy greater; sound his praise
    In thy eternal course, both when thou climb'st,
    And when high noon hast gained, and when thou fall'st.
    Moon, that now meet'st the orient Sun, now fliest
    With the fixed stars, fixed in their orb that flies;
    And ye five other wandering Fires, that move
    In mystic dance, not without song, resound
    His praise, who out of darkness called up Light.--v. 166-79.

Milton's conception of celestial distances, and of the vast regions of
interstellar space, is finely described in the following lines:--

                        Down thither prone in flight
    He speeds, and through the vast ethereal sky
    Sails between worlds and worlds, with steady wing
    Now on the polar winds; then with quick fan
    Winnows the buxom air, till, within soar
    Of towering eagles.--v. 266-71.

As in their morning, so in their evening devotions, our first parents
never fail to introduce a reference to the celestial orbs as indicating
the power and goodness of the Creator, made manifest in the beauty and
greatness of His works--

    Thus, at their shady lodge arrived, both stood,
    Both turned, and under open sky adored
    The God that made both Sky, Air, Earth and Heaven
    Which they beheld; the Moon's resplendent globe,
    And starry pole.--iv. 720-24.

The numerous extracts contained in this volume impress upon one's mind
how largely astronomy enters into the composition of 'Paradise Lost,'
and of how much assistance the knowledge of this science was to Milton
in the elaboration of his poem. Indeed, it would be hard to imagine how
such a work could have been written except by a poet who possessed a
proficient and comprehensive knowledge of astronomy. The chief
characteristic of Milton's poetry is its sublimity, which is the natural
outcome of the magnificence of his conceptions and of his own pure
imaginative genius. Among all the fields of literature, science, and
philosophy explored by him, he found none more congenial to his tastes,
or that afforded his imagination more freedom for its loftiest flights,
than the sublimest of sciences--astronomy. Whether we admire most the
accuracy of his astronomical knowledge, or the wonderful creations of
his poetic fancy, or his beautiful descriptions of the celestial orbs,
it is apparent that in this domain of science, as a poet, he stands
alone and without a rival. In his choice of the Ptolemaic cosmology
Milton adopted a system with which he had been familiar from his
youth--the same which his favourite poet Dante introduced into his poem,
'The Divina Commedia,' and which was well adapted for poetic
description. The picturesque conception of ten revolving spheres,
carrying along with them the orbs assigned to each, which, by their
revolution round the steadfast Earth, brought about with unfailing
regularity the successive alternation of day and night, and in every
twenty-four hours exhibited the pleasing vicissitudes of dawn, of
sunshine, of twilight, and of darkness, relieved by the soft effulgence
of the nocturnal sky, afforded Milton a favourable basis upon which to
construct a cosmical epic. The Copernican theory--with which he was
equally conversant, and in the accuracy and truthfulness of which he
believed--though less complicated than the Ptolemaic in its details, did
not possess the same attractiveness for poetic description that belonged
to the older system. According to this theory there is, surrounding us
on all sides, a boundless uncircumscribed ocean of space, to which it is
impossible to assign any conceivable limit; in every effort to
comprehend its dimensions or fathom its depths, the mind recoils upon
itself, baffled and discomfited, with a conscious feeling that there can
be no nearer approach to the end when end there is none that can be
conceived of. Interspersed throughout the regions of this azure vast of
space is the stellar universe, which to our comprehension is as infinite
as the abyss in which it exists. The solar system, though of magnificent
dimensions, is but a unit in the astronomical whole, in which are
embraced millions of other similar units--other solar systems, perhaps
differing in construction from that of ours, with billions of miles of
interstellar space intervening between each; yet so vast are the
dimensions of the celestial sphere that those distances when measured
upon it sink into utter insignificance. As the receding depths of space
are penetrated by powerful telescopes, they are found to be pervaded
with stars and starry archipelagoes, distributed in profusion over the
circular immensity and extending away into abysmal depths, beyond the
reach of visibility by any optical means which we possess. To the
universe there is no known end--nowhere in imagination can its boundary
be reached! This bewildering conception of the cosmos did not trouble
the minds of pre-Copernican thinkers. They regarded the steadfast Earth
as the most important body in the universe; nor were the celestial orbs
which circled round it believed to be very far distant. Tycho Brahé
imagined that the stars were not much more remote than the planets.
Epicurus thought the stars were small crystal mirrors in the sky which
reflected the solar rays, and the Venerable Bede remarked that they
needed assistance from the Sun's light in order to render them more
luminous.

The adoption of the Ptolemaic system by Milton afforded greater scope
for the exercise of his imaginative powers, and enabled him to bring
within the mental grasp of his readers a conception of the universe
which was not lost in the immensity associated with the Copernican view
of things. Besides, it also furnished him with a distinctly defined
basis upon which to erect the superstructure of his poem. Above the
circumscribed universe was Heaven or the Empyrean; underneath it was
Chaos, from which it had been reclaimed, and in the lowest depth of
which Milton located the infernal world called Hell. These four regions
embraced universal space; and in the elaboration of his great epic
Milton relied upon his imaginative genius, his brilliant scholarship,
his vast erudition, and the divine inspiration of the heavenly muse.
With these, aided by the power and vigour of his intellect, he was
enabled to produce a cosmical epic that surpassed all previous efforts
of a similar kind, and which still remains without a parallel.

One of the distinguishing features of Milton's mind was his wonderful
imagination, and in its exercise he beheld those sublime celestial and
terrestrial visions on which he reared fabrics of splendour and beauty,
described in harmonious numbers with the fervid eloquence and charm of a
true poet. An example of the loftiness and originality of his
imagination is afforded us in his description of the Creation, the main
facts of which he derived from the first two chapters of Genesis, and
upon these he elaborated in full and striking detail his magnificent
conception of the efforts of Divine Might, which in six successive
creative acts called into existence the universe and all that it
contains. The rising of the Earth out of Chaos; the creation of light
and of the orbs of the firmament; the joyfulness associated with the
onward career of the new-born Sun; the subdued illumination of the
full-orbed Moon, and the thousand thousand stars that spangle the
nocturnal sky--all these afforded Milton a rich field in which his
imagination luxuriated, and in the description of which he found
subject-matter worthy of his gifted intellect.

Milton gives an ampler and more detailed description of the new universe
in his narration of Satan's journey through space in search of this
world, and brings more vividly before the imagination of his readers the
glories of the celestial regions. The fiend, having emerged from the
dark abyss of Chaos into a region of light, first beheld the new
creation from such a distance that to his view it appeared as a star
suspended by a golden chain from the Empyrean. This stellar conception
of the poet's harmonised with the views of the Ptolemaists, who believed
that the universe was of limited extent, and though its dimensions were
vast beyond comprehension, it was, nevertheless, enclosed by the tenth
sphere or Primum Mobile. It was on the surface of this sphere that Satan
alighted, and over which he wandered, until attracted by a beam of light
that appeared through an opening at its zenith, where, by means of a
stair or ladder, communication was maintained between the new universe
and Heaven above. Hither the undaunted fiend hied, and, standing on the
lower steps of this structure, momentarily paused to gaze upon the
glorious sight which burst upon his view before directing his flight
down into the newly created universe. Milton then describes his progress
through the stellar regions, his landing in the Sun and what he saw
there, and the termination of his journey when he descends from the
ecliptic down to the Earth. In doing so the poet gives a wonderfully
beautiful description of the starry universe, of the Sun, Moon, and
Earth (Book III. 540-742), enhanced and adorned with his own poetic
imaginings derived from fable, philosophy, and science.

Milton makes more frequent allusion to the Sun than to any of the other
orbs of the firmament. This we should expect: the poet always gives the
orb the precedence which is his due, and never fails, when the occasion
requires it, to surround him with the 'surpassing glory' which marks his
pre-eminence above all other occupants of the sky. The Moon, his
consort--peerless in the subdued effulgence of her borrowed light; the
beautiful star of evening, Hesperus; the sidereal heavens with their
untold glories; the Galaxy, overpowering in the magnificence of its
clouds and streams of stars--all these have their beauties and charms
mirrored in the pages of this remarkable poem.

That the observation of the celestial orbs, their phases, and the varied
phenomena which occur as a consequence of their motions, were to Milton
an unfailing source of enjoyment and of meditative delight, is evident
from the frequency with which he alludes to them. The following lines
also testify to this:--

    For wonderful indeed are all his works,
    Pleasant to know, and worthiest to be all
    Had in remembrance always with delight!
    But what created mind can comprehend
    Their number, or the wisdom infinite
    That brought them forth, but hid their causes deep?--iii. 703-708.

It is very pleasant, as Milton says, to

                        sit and rightly spell
    Of every star that heaven doth show.

It is also pleasant to know the astronomy of his 'Paradise Lost,' and to
linger over the delightful and harmonious utterances associated with the
sublimest of sciences, expressed in the melodious language of England's
greatest epic poet.


              PRINTED BY
SPOTTISWOODE AND CO., NEW-STREET SQUARE
                LONDON




FOOTNOTES:


[1] Chambers's _Handbook of Astronomy_.

[2] Brewster's _Martyrs of Science_.

[3] The transit occurred on a Sunday, and the 'business of the highest
importance' to which Horrox alludes was his clerical duties.

[4] A fresco by the late Mr. Ford Maddox-Brown, depicting Crabtree
observing the transit of Venus, adorns the interior of the Manchester
Town Hall.

[5] William Crabtree died on August 1, 1644, aged 34 years.

[6] The constellation Virgo.

[7] _Life of Galileo_ (Library of Useful Knowledge).

[8] Miss Clerke's _System of the Stars_.

[9] Miss Clerke's _System of the Stars_.

[10] Miss Clerke's _System of the Stars_.

[11] _Ibid._

[12] An expression in Book VIII. 148-49 would seem to indicate that this
was inaccurate, but the lines

                          'and other suns perhaps
    With their attendant moons, thou wilt descry,'

are an allusion to the planets Jupiter and Saturn, whose satellites had
been recently discovered.

[13] Mr. E. W. Maunder, in _Knowledge_, March 1894.

[14] Though not a celestial body, it is considered desirable to describe
the Earth as a member of the solar system.

[15] See diagram, chap. iii. p. 96.





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