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History of Astronomy by George Forbes

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[Illustration: SIR ISAAC NEWTON (From the bust by Roubiliac In Trinity
College, Cambridge.)]

HISTORY OF ASTRONOMY

BY

GEORGE FORBES,
M.A., F.R.S., M. INST. C. E.,

(FORMERLY PROFESSOR OF NATURAL PHILOSOPHY, ANDERSON'S COLLEGE, GLASGOW)

AUTHOR OF "THE TRANSIT OF VENUS," RENDU'S "THEORY OF THE GLACIERS OF
SAVOY," ETC., ETC.

CONTENTS

PREFACE

BOOK I. THE GEOMETRICAL PERIOD

1. PRIMITIVE ASTRONOMY AND ASTROLOGY

2. ANCIENT ASTRONOMY--CHINESE AND CHALDAEANS

3. ANCIENT GREEK ASTRONOMY

4. THE REIGN OF EPICYCLES--FROM PTOLEMY TO COPERNICUS

BOOK II. THE DYNAMICAL PERIOD

5. DISCOVERY OF THE TRUE SOLAR SYSTEM--TYCHO BRAHE--KEPLER

6. GALILEO AND THE TELESCOPE--NOTIONS OF GRAVITY BY HORROCKS, ETC.

7. SIR ISAAC NEWTON--LAW OF UNIVERSAL GRAVITATION

8. NEWTON'S SUCCESSORS--HALLEY, EULER, LAGRANGE, LAPLACE, ETC.

9. DISCOVERY OF NEW PLANETS--HERSCHEL, PIAZZI, ADAMS, AND LE
VERRIER

BOOK III. OBSERVATION

10. INSTRUMENTS OF PRECISION--SIZE OF THE SOLAR SYSTEM

11. HISTORY OF THE TELESCOPE--SPECTROSCOPE

BOOK IV. THE PHYSICAL PERIOD

12. THE SUN

13. THE MOON AND PLANETS

14. COMETS AND METEORS

15. THE STARS AND NEBULAE

INDEX

PREFACE

An attempt has been made in these pages to trace the evolution of
intellectual thought in the progress of astronomical discovery, and,
by recognising the different points of view of the different ages, to
give due credit even to the ancients. No one can expect, in a history
of astronomy of limited size, to find a treatise on "practical" or on
"theoretical astronomy," nor a complete "descriptive astronomy," and
still less a book on "speculative astronomy." Something of each of
these is essential, however, for tracing the progress of thought and
knowledge which it is the object of this History to describe.

The progress of human knowledge is measured by the increased habit of
looking at facts from new points of view, as much as by the
accumulation of facts. The mental capacity of one age does not seem to
differ from that of other ages; but it is the imagination of new
points of view that gives a wider scope to that capacity. And this is
cumulative, and therefore progressive. Aristotle viewed the solar
system as a geometrical problem; Kepler and Newton converted the point
of view into a dynamical one. Aristotle's mental capacity to
understand the meaning of facts or to criticise a train of reasoning
may have been equal to that of Kepler or Newton, but the point of view
was different.

Then, again, new points of view are provided by the invention of new
methods in that system of logic which we call mathematics. All that
mathematics can do is to assure us that a statement A is equivalent to
statements B, C, D, or is one of the facts expressed by the statements
B, C, D; so that we may know, if B, C, and D are true, then A is true.
To many people our inability to understand all that is contained in
statements B, C, and D, without the cumbrous process of a mathematical
demonstration, proves the feebleness of the human mind as a logical
machine. For it required the new point of view imagined by Newton's
analysis to enable people to see that, so far as planetary orbits are
concerned, Kepler's three laws (B, C, D) were identical with Newton's
law of gravitation (A). No one recognises more than the mathematical
astronomer this feebleness of the human intellect, and no one is more
conscious of the limitations of the logical process called
mathematics, which even now has not solved directly the problem of
only three bodies.

These reflections, arising from the writing of this History, go to
explain the invariable humility of the great mathematical astronomers.
Newton's comparison of himself to the child on the seashore applies to
them all. As each new discovery opens up, it may be, boundless oceans
for investigation, for wonder, and for admiration, the great
astronomers, refusing to accept mere hypotheses as true, have founded
upon these discoveries a science as exact in its observation of facts
as in theories. So it is that these men, who have built up the most
sure and most solid of all the sciences, refuse to invite others to
join them in vain speculation. The writer has, therefore, in this
short History, tried to follow that great master, Airy, whose pupil he
was, and the key to whose character was exactness and accuracy; and he
recognises that Science is impotent except in her own limited sphere.

It has been necessary to curtail many parts of the History in the
attempt--perhaps a hopeless one--to lay before the reader in a limited
space enough about each age to illustrate its tone and spirit, the
ideals of the workers, the gradual addition of new points of view and
of new means of investigation.

It would, indeed, be a pleasure to entertain the hope that these pages
might, among new recruits, arouse an interest in the greatest of all
the sciences, or that those who have handled the theoretical or
practical side might be led by them to read in the original some of
the classics of astronomy. Many students have much compassion for the
schoolboy of to-day, who is not allowed the luxury of learning the art
of reasoning from him who still remains pre-eminently its greatest
exponent, Euclid. These students pity also the man of to-morrow, who
is not to be allowed to read, in the original Latin of the brilliant
Kepler, how he was able--by observations taken from a moving platform,
the earth, of the directions of a moving object, Mars--to deduce the
exact shape of the path of each of these planets, and their actual
positions on these paths at any time. Kepler's masterpiece is one of
the most interesting books that was ever written, combining wit,
imagination, ingenuity, and certainty.

Lastly, it must be noted that, as a History of England cannot deal
with the present Parliament, so also the unfinished researches and
untested hypotheses of many well-known astronomers of to-day cannot be
included among the records of the History of Astronomy. The writer
regrets the necessity that thus arises of leaving without mention the
names of many who are now making history in astronomical work.

G. F.
_August 1st, 1909._

BOOK I. THE GEOMETRICAL PERIOD

1. PRIMITIVE ASTRONOMY AND ASTROLOGY.

The growth of intelligence in the human race has its counterpart in
that of the individual, especially in the earliest stages.
Intellectual activity and the development of reasoning powers are in
both cases based upon the accumulation of experiences, and on the
comparison, classification, arrangement, and nomenclature of these
experiences. During the infancy of each the succession of events can
be watched, but there can be no _a priori_ anticipations.
Experience alone, in both cases, leads to the idea of cause and effect
as a principle that seems to dominate our present universe, as a rule
for predicting the course of events, and as a guide to the choice of a
course of action. This idea of cause and effect is the most potent
factor in developing the history of the human race, as of the
individual.

In no realm of nature is the principle of cause and effect more
conspicuous than in astronomy; and we fall into the habit of thinking
of its laws as not only being unchangeable in our universe, but
necessary to the conception of any universe that might have been
substituted in its place. The first inhabitants of the world were
compelled to accommodate their acts to the daily and annual
alternations of light and darkness and of heat and cold, as much as to
the irregular changes of weather, attacks of disease, and the fortune
of war. They soon came to regard the influence of the sun, in
connection with light and heat, as a cause. This led to a search for
other signs in the heavens. If the appearance of a comet was sometimes
noted simultaneously with the death of a great ruler, or an eclipse
with a scourge of plague, these might well be looked upon as causes in
the same sense that the veering or backing of the wind is regarded as
a cause of fine or foul weather.

For these reasons we find that the earnest men of all ages have
recorded the occurrence of comets, eclipses, new stars, meteor
showers, and remarkable conjunctions of the planets, as well as
plagues and famines, floods and droughts, wars and the deaths of great
rulers. Sometimes they thought they could trace connections which
might lead them to say that a comet presaged famine, or an eclipse
war.

Even if these men were sometimes led to evolve laws of cause and
effect which now seem to us absurd, let us be tolerant, and gratefully
acknowledge that these astrologers, when they suggested such "working
hypotheses," were laying the foundations of observation and deduction.

If the ancient Chaldaeans gave to the planetary conjunctions an
influence over terrestrial events, let us remember that in our own
time people have searched for connection between terrestrial
conditions and periods of unusual prevalence of sun spots; while De la
Rue, Loewy, and Balfour Stewart[1] thought they found a connection
between sun-spot displays and the planetary positions. Thus we find
scientific men, even in our own time, responsible for the belief that
storms in the Indian Ocean, the fertility of German vines, famines in
India, and high or low Nile-floods in Egypt follow the planetary
positions.

And, again, the desire to foretell the weather is so laudable that we
cannot blame the ancient Greeks for announcing the influence of the
moon with as much confidence as it is affirmed in Lord Wolseley's
_Soldier's Pocket Book_.

Even if the scientific spirit of observation and deduction (astronomy)
has sometimes led to erroneous systems for predicting terrestrial
events (astrology), we owe to the old astronomer and astrologer alike
the deepest gratitude for their diligence in recording astronomical
events. For, out of the scanty records which have survived the
destructive acts of fire and flood, of monarchs and mobs, we have
found much that has helped to a fuller knowledge of the heavenly
motions than was possible without these records.

So Hipparchus, about 150 B.C., and Ptolemy a little later, were able
to use the observations of Chaldaean astrologers, as well as those of
Alexandrian astronomers, and to make some discoveries which have
helped the progress of astronomy in all ages. So, also, Mr. Cowell[2]
has examined the marks made on the baked bricks used by the Chaldaeans
for recording the eclipses of 1062 B.C. and 762 B.C.; and has thereby
been enabled, in the last few years, to correct the lunar tables of
Hansen, and to find a more accurate value for the secular acceleration
of the moon's longitude and the node of her orbit than any that could
be obtained from modern observations made with instruments of the
highest precision.

So again, Mr. Hind [3] was enabled to trace back the period during
which Halley's comet has been a member of the solar system, and to
identify it in the Chinese observations of comets as far back as 12
B.C. Cowell and Cromellin extended the date to 240 B.C. In the same
way the comet 1861.i. has been traced back in the Chinese records to
617 A.D. [4]

The theoretical views founded on Newton's great law of universal
gravitation led to the conclusion that the inclination of the earth's
equator to the plane of her orbit (the obliquity of the ecliptic) has
been diminishing slowly since prehistoric times; and this fact has
been confirmed by Egyptian and Chinese observations on the length of
the shadow of a vertical pillar, made thousands of years before the
Christian era, in summer and winter.

There are other reasons why we must be tolerant of the crude notions
of the ancients. The historian, wishing to give credit wherever it may
be due, is met by two difficulties. Firstly, only a few records of
very ancient astronomy are extant, and the authenticity of many of
these is open to doubt. Secondly, it is very difficult to divest
ourselves of present knowledge, and to appreciate the originality of
thought required to make the first beginnings.

With regard to the first point, we are generally dependent upon
histories written long after the events. The astronomy of Egyptians,
Babylonians, and Assyrians is known to us mainly through the Greek
historians, and for information about the Chinese we rely upon the
researches of travellers and missionaries in comparatively recent
times. The testimony of the Greek writers has fortunately been
confirmed, and we now have in addition a mass of facts translated from
the original sculptures, papyri, and inscribed bricks, dating back
thousands of years.

In attempting to appraise the efforts of the beginners we must
remember that it was natural to look upon the earth (as all the first
astronomers did) as a circular plane, surrounded and bounded by the
heaven, which was a solid vault, or hemisphere, with its concavity
turned downwards. The stars seemed to be fixed on this vault; the
moon, and later the planets, were seen to crawl over it. It was a
great step to look on the vault as a hollow sphere carrying the sun
too. It must have been difficult to believe that at midday the stars
are shining as brightly in the blue sky as they do at night. It must
have been difficult to explain how the sun, having set in the west,
could get back to rise in the east without being seen _if_ it was
always the same sun. It was a great step to suppose the earth to be
spherical, and to ascribe the diurnal motions to its rotation.
Probably the greatest step ever made in astronomical theory was the
placing of the sun, moon, and planets at different distances from the
earth instead of having them stuck on the vault of heaven. It was a
transition from "flatland" to a space of three dimensions.

Great progress was made when systematic observations began, such as
following the motion of the moon and planets among the stars, and the
inferred motion of the sun among the stars, by observing their
_heliacal risings_--i.e., the times of year when a star
would first be seen to rise at sunrise, and when it could last be seen
to rise at sunset. The grouping of the stars into constellations and
recording their places was a useful observation. The theoretical
prediction of eclipses of the sun and moon, and of the motions of the
planets among the stars, became later the highest goal in astronomy.

To not one of the above important steps in the progress of astronomy
can we assign the author with certainty. Probably many of them were
independently taken by Chinese, Indian, Persian, Tartar, Egyptian,
Babylonian, Assyrian, Phoenician, and Greek astronomers. And we have
not a particle of information about the discoveries, which may have
been great, by other peoples--by the Druids, the Mexicans, and the
Peruvians, for example.

We do know this, that all nations required to have a calendar. The
solar year, the lunar month, and the day were the units, and it is
owing to their incommensurability that we find so many calendars
proposed and in use at different times. The only object to be attained
by comparing the chronologies of ancient races is to fix the actual
dates of observations recorded, and this is not a part of a history of
astronomy.

In conclusion, let us bear in mind the limited point of view of the
ancients when we try to estimate their merit. Let us remember that the
first astronomy was of two dimensions; the second astronomy was of
three dimensions, but still purely geometrical. Since Kepler's day we
have had a dynamical astronomy.

FOOTNOTES:

[1] Trans. R. S. E., xxiii. 1864, p. 499, _On Sun Spots_, etc., by
B. Stewart. Also Trans. R. S. 1860-70. Also Prof. Ernest Brown, in
_R. A. S. Monthly Notices_, 1900.

[2] _R. A. S. Monthly Notices_, Sup.; 1905.

[Illustration: CHALDAEAN BAKED BRICK OR TABLET, _Obverse and reverse
sides_, Containing record of solar eclipse, 1062 B.C., used lately by
Cowell for rendering the lunar theory more accurate than was possible
by finest modern observations. (British Museum collection,
No. 35908.)]

[3] _R. A. S. Monthly Notices_, vol. x., p. 65.

[4] R. S. E. Proc., vol. x., 1880.

2. ANCIENT ASTRONOMY--THE CHINESE AND CHALDAEANS.

The last section must have made clear the difficulties the way of
assigning to the ancient nations their proper place in the development
of primitive notions about astronomy. The fact that some alleged
observations date back to a period before the Chinese had invented the
art of writing leads immediately to the question how far tradition can
be trusted.

Our first detailed knowledge was gathered in the far East by
travellers, and by the Jesuit priests, and was published in the
eighteenth century. The Asiatic Society of Bengal contributed
translations of Brahmin literature. The two principal sources of
knowledge about Chinese astronomy were supplied, first by Father
Souciet, who in 1729 published _Observations Astronomical,
Geographical, Chronological, and Physical_, drawn from ancient
Chinese books; and later by Father Moyriac-de-Mailla, who in 1777-1785
published _Annals of the Chinese Empire, translated from
Tong-Kien-Kang-Mou_.

Bailly, in his _Astronomie Ancienne_ (1781), drew, from these and
other sources, the conclusion that all we know of the astronomical
learning of the Chinese, Indians, Chaldaeans, Assyrians, and Egyptians
is but the remnant of a far more complete astronomy of which no trace
can be found.

Delambre, in his _Histoire de l'Astronomie Ancienne_ (1817),
ridicules the opinion of Bailly, and considers that the progress made
by all of these nations is insignificant.

It will be well now to give an idea of some of the astronomy of the
ancients not yet entirely discredited. China and Babylon may be taken
as typical examples.

_China_.--It would appear that Fohi, the first emperor, reigned
about 2952 B.C., and shortly afterwards Yu-Chi made a sphere to
represent the motions of the celestial bodies. It is also mentioned,
in the book called Chu-King, supposed to have been written in 2205
B.C., that a similar sphere was made in the time of Yao (2357
B.C.).[1] It is said that the Emperor Chueni (2513 B.C.) saw five
planets in conjunction the same day that the sun and moon were in
conjunction. This is discussed by Father Martin (MSS. of De Lisle);
also by M. Desvignolles (Mem. Acad. Berlin, vol. iii., p. 193), and by
M. Kirsch (ditto, vol. v., p. 19), who both found that Mars, Jupiter,
Saturn, and Mercury were all between the eleventh and eighteenth
degrees of Pisces, all visible together in the evening on February
28th 2446 B.C., while on the same day the sun and moon were in
conjunction at 9 a.m., and that on March 1st the moon was in
conjunction with the other four planets. But this needs confirmation.

Yao, referred to above, gave instructions to his astronomers to
determine the positions of the solstices and equinoxes, and they
reported the names of the stars in the places occupied by the sun at
these seasons, and in 2285 B.C. he gave them further orders. If this
account be true, it shows a knowledge that the vault of heaven is a
complete sphere, and that stars are shining at mid-day, although
eclipsed by the sun's brightness.

It is also asserted, in the book called _Chu-King_, that in the
time of Yao the year was known to have 365-1/4 days, and that he
adopted 365 days and added an intercalary day every four years (as in
the Julian Calendar). This may be true or not, but the ancient Chinese
certainly seem to have divided the circle into 365 degrees. To learn
the length of the year needed only patient observation--a
characteristic of the Chinese; but many younger nations got into a
terrible mess with their calendar from ignorance of the year's length.

It is stated that in 2159 B.C. the royal astronomers Hi and Ho failed
to predict an eclipse. It probably created great terror, for they were
executed in punishment for their neglect. If this account be true, it
means that in the twenty-second century B.C. some rule for calculating
eclipses was in use. Here, again, patient observation would easily
lead to the detection of the eighteen-year cycle known to the
Chaldeans as the _Saros_. It consists of 235 lunations, and in
that time the pole of the moon's orbit revolves just once round the
pole of the ecliptic, and for this reason the eclipses in one cycle
are repeated with very slight modification in the next cycle, and so
on for many centuries.

It may be that the neglect of their duties by Hi and Ho, and their
punishment, influenced Chinese astronomy; or that the succeeding
records have not been available to later scholars; but the fact
remains that--although at long intervals observations were made of
eclipses, comets, and falling stars, and of the position of the
solstices, and of the obliquity of the ecliptic--records become rare,
until 776 B.C., when eclipses began to be recorded once more with some
approach to continuity. Shortly afterwards notices of comets were
added. Biot gave a list of these, and Mr. John Williams, in 1871,
published _Observations of Comets from 611 B.C. to 1640 A.D.,
Extracted from the Chinese Annals_.

With regard to those centuries concerning which we have no
astronomical Chinese records, it is fair to state that it is recorded
that some centuries before the Christian era, in the reign of
Tsin-Chi-Hoang, all the classical and scientific books that could be
found were ordered to be destroyed. If true, our loss therefrom is as
great as from the burning of the Alexandrian library by the Caliph
Omar. He burnt all the books because he held that they must be either
consistent or inconsistent with the Koran, and in the one case they
were superfluous, in the other case objectionable.

_Chaldaeans_.--Until the last half century historians were
accustomed to look back upon the Greeks, who led the world from the
fifth to the third century B.C., as the pioneers of art, literature,
and science. But the excavations and researches of later years make us
more ready to grant that in science as in art the Greeks only
developed what they derived from the Egyptians, Babylonians, and
Assyrians. The Greek historians said as much, in fact; and modern
commentators used to attribute the assertion to undue modesty. Since,
however, the records of the libraries have been unearthed it has been
recognised that the Babylonians were in no way inferior in the matter
of original scientific investigation to other races of the same era.

The Chaldaeans, being the most ancient Babylonians, held the same
station and dignity in the State as did the priests in Egypt, and
spent all their time in the study of philosophy and astronomy, and the
arts of divination and astrology. They held that the world of which we
have a conception is an eternal world without any beginning or ending,
in which all things are ordered by rules supported by a divine
providence, and that the heavenly bodies do not move by chance, nor by
their own will, but by the determinate will and appointment of the
gods. They recorded these movements, but mainly in the hope of tracing
the will of the gods in mundane affairs. Ptolemy (about 130 A.D.)
made use of Babylonian eclipses in the eighth century B.C. for
improving his solar and lunar tables.

Fragments of a library at Agade have been preserved at Nineveh, from
which we learn that the star-charts were even then divided into
constellations, which were known by the names which they bear to this
day, and that the signs of the zodiac were used for determining the
courses of the sun, moon, and of the five planets Mercury, Venus,
Mars, Jupiter, and Saturn.

We have records of observations carried on under Asshurbanapal, who
sent astronomers to different parts to study celestial phenomena. Here
is one:--

To the Director of Observations,--My Lord, his humble servant
Nabushum-iddin, Great Astronomer of Nineveh, writes thus: "May Nabu
and Marduk be propitious to the Director of these Observations, my
Lord. The fifteenth day we observed the Node of the moon, and the moon
was eclipsed."

The Phoenicians are supposed to have used the stars for navigation,
but there are no records. The Egyptian priests tried to keep such
astronomical knowledge as they possessed to themselves. It is probable
that they had arbitrary rules for predicting eclipses. All that was
known to the Greeks about Egyptian science is to be found in the
writings of Diodorus Siculus. But confirmatory and more authentic
facts have been derived from late explorations. Thus we learn from
E. B. Knobel[2] about the Jewish calendar dates, on records of land
sales in Aramaic papyri at Assuan, translated by Professor A. H. Sayce
and A. E. Cowley, (1) that the lunar cycle of nineteen years was used
by the Jews in the fifth century B.C. [the present reformed Jewish
calendar dating from the fourth century A.D.], a date a "little more
than a century after the grandfathers and great-grandfathers of those
whose business is recorded had fled into Egypt with Jeremiah" (Sayce);
and (2) that the order of intercalation at that time was not
dissimilar to that in use at the present day.

Then again, Knobel reminds us of "the most interesting discovery a few
years ago by Father Strassmeier of a Babylonian tablet recording a
partial lunar eclipse at Babylon in the seventh year of Cambyses, on
the fourteenth day of the Jewish month Tammuz." Ptolemy, in the
Almagest (Suntaxis), says it occurred in the seventh year of Cambyses,
on the night of the seventeenth and eighteenth of the Egyptian month
Phamenoth. Pingre and Oppolzer fix the date July 16th, 533 B.C. Thus
are the relations of the chronologies of Jews and Egyptians
established by these explorations.

FOOTNOTES:

[1] These ancient dates are uncertain.

[2] _R. A. S. Monthly Notices_, vol. lxviii., No. 5, March, 1908.

3. ANCIENT GREEK ASTRONOMY.

We have our information about the earliest Greek astronomy from
Herodotus (born 480 B.C.). He put the traditions into writing. Thales
(639-546 B.C.) is said to have predicted an eclipse, which caused much
alarm, and ended the battle between the Medes and Lydians. Airy fixed
the date May 28th, 585 B.C. But other modern astronomers give
different dates. Thales went to Egypt to study science, and learnt
from its priests the length of the year (which was kept a profound
secret!), and the signs of the zodiac, and the positions of the
solstices. He held that the sun, moon, and stars are not mere spots on
the heavenly vault, but solids; that the moon derives her light from
the sun, and that this fact explains her phases; that an eclipse of
the moon happens when the earth cuts off the sun's light from her. He
supposed the earth to be flat, and to float upon water. He determined
the ratio of the sun's diameter to its orbit, and apparently made out
the diameter correctly as half a degree. He left nothing in writing.

His successors, Anaximander (610-547 B.C.) and Anaximenes (550-475
B.C.), held absurd notions about the sun, moon, and stars, while
Heraclitus (540-500 B.C.) supposed that the stars were lighted each
night like lamps, and the sun each morning. Parmenides supposed the
earth to be a sphere.

Pythagoras (569-470 B.C.) visited Egypt to study science. He deduced
his system, in which the earth revolves in an orbit, from fantastic
first principles, of which the following are examples: "The circular
motion is the most perfect motion," "Fire is more worthy than earth,"
"Ten is the perfect number." He wrote nothing, but is supposed to have
said that the earth, moon, five planets, and fixed stars all revolve
round the sun, which itself revolves round an imaginary central fire
called the Antichthon. Copernicus in the sixteenth century claimed
Pythagoras as the founder of the system which he, Copernicus, revived.

Anaxagoras (born 499 B.C.) studied astronomy in Egypt. He explained
the return of the sun to the east each morning by its going under the
flat earth in the night. He held that in a solar eclipse the moon
hides the sun, and in a lunar eclipse the moon enters the earth's
shadow--both excellent opinions. But he entertained absurd ideas of
the vortical motion of the heavens whisking stones into the sky, there
to be ignited by the fiery firmament to form stars. He was prosecuted
for this unsettling opinion, and for maintaining that the moon is an
inhabited earth. He was defended by Pericles (432 B.C.).

Solon dabbled, like many others, in reforms of the calendar. The
common year of the Greeks originally had 360 days--twelve months of
thirty days. Solon's year was 354 days. It is obvious that these
erroneous years would, before long, remove the summer to January and
the winter to July. To prevent this it was customary at regular
intervals to intercalate days or months. Meton (432 B.C.) introduced a
reform based on the nineteen-year cycle. This is not the same as the
Egyptian and Chaldean eclipse cycle called _Saros_ of 223
lunations, or a little over eighteen years. The Metonic cycle is 235
lunations or nineteen years, after which period the sun and moon
occupy the same position relative to the stars. It is still used for
fixing the date of Easter, the number of the year in Melon's cycle
being the golden number of our prayer-books. Melon's system divided
the 235 lunations into months of thirty days and omitted every
sixty-third day. Of the nineteen years, twelve had twelve months and
seven had thirteen months.

Callippus (330 B.C.) used a cycle four times as long, 940 lunations,
but one day short of Melon's seventy-six years. This was more correct.

Eudoxus (406-350 B.C.) is said to have travelled with Plato in
Egypt. He made astronomical observations in Asia Minor, Sicily, and
Italy, and described the starry heavens divided into constellations.
His name is connected with a planetary theory which as generally
stated sounds most fanciful. He imagined the fixed stars to be on a
vault of heaven; and the sun, moon, and planets to be upon similar
vaults or spheres, twenty-six revolving spheres in all, the motion of
each planet being resolved into its components, and a separate sphere
being assigned for each component motion. Callippus (330 B.C.)
increased the number to thirty-three. It is now generally accepted
that the real existence of these spheres was not suggested, but the
idea was only a mathematical conception to facilitate the construction
of tables for predicting the places of the heavenly bodies.

Aristotle (384-322 B.C.) summed up the state of astronomical knowledge
in his time, and held the earth to be fixed in the centre of the
world.

Nicetas, Heraclides, and Ecphantes supposed the earth to revolve on
its axis, but to have no orbital motion.

The short epitome so far given illustrates the extraordinary deductive
methods adopted by the ancient Greeks. But they went much farther in
the same direction. They seem to have been in great difficulty to
explain how the earth is supported, just as were those who invented
the myth of Atlas, or the Indians with the tortoise. Thales thought
that the flat earth floated on water. Anaxagoras thought that, being
flat, it would be buoyed up and supported on the air like a kite.
Democritus thought it remained fixed, like the donkey between two
bundles of hay, because it was equidistant from all parts of the
containing sphere, and there was no reason why it should incline one
way rather than another. Empedocles attributed its state of rest to
centrifugal force by the rapid circular movement of the heavens, as
water is stationary in a pail when whirled round by a string.
Democritus further supposed that the inclination of the flat earth to
the ecliptic was due to the greater weight of the southern parts owing
to the exuberant vegetation.

For further references to similar efforts of imagination the reader is
referred to Sir George Cornwall Lewis's _Historical Survey of the
Astronomy of the Ancients_; London, 1862. His list of authorities
is very complete, but some of his conclusions are doubtful. At p. 113
of that work he records the real opinions of Socrates as set forth by
Xenophon; and the reader will, perhaps, sympathise with Socrates in
his views on contemporary astronomy:--

With regard to astronomy he [Socrates] considered a knowledge of it
desirable to the extent of determining the day of the year or month,
and the hour of the night, ... but as to learning the courses of the
stars, to be occupied with the planets, and to inquire about their
distances from the earth, and their orbits, and the causes of their
motions, he strongly objected to such a waste of valuable time. He
dwelt on the contradictions and conflicting opinions of the physical
philosophers, ... and, in fine, he held that the speculators on the
universe and on the laws of the heavenly bodies were no better than
madmen (_Xen. Mem_, i. 1, 11-15).

Plato (born 429 B.C.), the pupil of Socrates, the fellow-student of
Euclid, and a follower of Pythagoras, studied science in his travels
in Egypt and elsewhere. He was held in so great reverence by all
learned men that a problem which he set to the astronomers was the
keynote to all astronomical investigation from this date till the time
of Kepler in the sixteenth century. He proposed to astronomers _the
problem of representing the courses of the planets by circular and
uniform motions_.

Systematic observation among the Greeks began with the rise of the
Alexandrian school. Aristillus and Timocharis set up instruments and
fixed the positions of the zodiacal stars, near to which all the
planets in their orbits pass, thus facilitating the determination of
planetary motions. Aristarchus (320-250 B.C.) showed that the sun must
be at least nineteen times as far off as the moon, which is far short
of the mark. He also found the sun's diameter, correctly, to be half a
degree. Eratosthenes (276-196 B.C.) measured the inclination to the
equator of the sun's apparent path in the heavens--i.e., he measured
the obliquity of the ecliptic, making it 23 degrees 51', confirming
our knowledge of its continuous diminution during historical times. He
measured an arc of meridian, from Alexandria to Syene (Assuan), and
found the difference of latitude by the length of a shadow at noon,
summer solstice. He deduced the diameter of the earth, 250,000
stadia. Unfortunately, we do not know the length of the stadium he
used.

Hipparchus (190-120 B.C.) may be regarded as the founder of
observational astronomy. He measured the obliquity of the ecliptic,
and agreed with Eratosthenes. He altered the length of the tropical
year from 365 days, 6 hours to 365 days, 5 hours, 53 minutes--still
four minutes too much. He measured the equation of time and the
irregular motion of the sun; and allowed for this in his calculations
by supposing that the centre, about which the sun moves uniformly, is
situated a little distance from the fixed earth. He called this point
the _excentric_. The line from the earth to the "excentric" was
called the _line of apses_. A circle having this centre was
called the _equant_, and he supposed that a radius drawn to the
sun from the excentric passes over equal arcs on the equant in equal
times. He then computed tables for predicting the place of the sun.

He proceeded in the same way to compute Lunar tables. Making use of
Chaldaean eclipses, he was able to get an accurate value of the moon's
mean motion. [Halley, in 1693, compared this value with his own
measurements, and so discovered the acceleration of the moon's mean
motion. This was conclusively established, but could not be explained
by the Newtonian theory for quite a long time.] He determined the
plane of the moon's orbit and its inclination to the ecliptic. The
motion of this plane round the pole of the ecliptic once in eighteen
years complicated the problem. He located the moon's excentric as he
had done the sun's. He also discovered some of the minor
irregularities of the moon's motion, due, as Newton's theory proves,
to the disturbing action of the sun's attraction.

In the year 134 B.C. Hipparchus observed a new star. This upset every
notion about the permanence of the fixed stars. He then set to work to
catalogue all the principal stars so as to know if any others appeared
or disappeared. Here his experiences resembled those of several later
astronomers, who, when in search of some special object, have been
rewarded by a discovery in a totally different direction. On comparing
his star positions with those of Timocharis and Aristillus he found no
stars that had appeared or disappeared in the interval of 150 years;
but he found that all the stars seemed to have changed their places
with reference to that point in the heavens where the ecliptic is 90
degrees from the poles of the earth--i.e., the equinox. He found that
this could be explained by a motion of the equinox in the direction of
the apparent diurnal motion of the stars. This discovery of
_precession of the equinoxes_, which takes place at the rate of 52".1
every year, was necessary for the progress of accurate astronomical
observations. It is due to a steady revolution of the earth's pole
round the pole of the ecliptic once in 26,000 years in the opposite
direction to the planetary revolutions.

Hipparchus was also the inventor of trigonometry, both plane and
spherical. He explained the method of using eclipses for determining
the longitude.

In connection with Hipparchus' great discovery it may be mentioned
that modern astronomers have often attempted to fix dates in history
by the effects of precession of the equinoxes. (1) At about the date
when the Great Pyramid may have been built gamma Draconis was near to
the pole, and must have been used as the pole-star. In the north face
of the Great Pyramid is the entrance to an inclined passage, and six
of the nine pyramids at Gizeh possess the same feature; all the
passages being inclined at an angle between 26 degrees and 27 degrees
to the horizon and in the plane of the meridian. It also appears that
4,000 years ago--i.e., about 2100 B.C.--an observer at the lower end
of the passage would be able to see gamma Draconis, the then
pole-star, at its lower culmination.[1] It has been suggested that the
passage was made for this purpose. On other grounds the date assigned
to the Great Pyramid is 2123 B.C.

(2) The Chaldaeans gave names to constellations now invisible from
Babylon which would have been visible in 2000 B.C., at which date it
is claimed that these people were studying astronomy.

(3) In the Odyssey, Calypso directs Odysseus, in accordance with
Phoenician rules for navigating the Mediterranean, to keep the Great
Bear "ever on the left as he traversed the deep" when sailing from the
pillars of Hercules (Gibraltar) to Corfu. Yet such a course taken now
would land the traveller in Africa. Odysseus is said in his voyage in
springtime to have seen the Pleiades and Arcturus setting late, which
seemed to early commentators a proof of Homer's inaccuracy. Likewise
Homer, both in the _Odyssey_ [2] (v. 272-5) and in the _Iliad_
(xviii. 489), asserts that the Great Bear never set in those
latitudes. Now it has been found that the precession of the equinoxes
explains all these puzzles; shows that in springtime on the
Mediterranean the Bear was just above the horizon, near the sea but
not touching it, between 750 B.C. and 1000 B.C.; and fixes the date of
the poems, thus confirming other evidence, and establishing Homer's
character for accuracy. [3]

(4) The orientation of Egyptian temples and Druidical stones is such
that possibly they were so placed as to assist in the observation of
the heliacal risings [4] of certain stars. If the star were known,
this would give an approximate date. Up to the present the results of
these investigations are far from being conclusive.

Ptolemy (130 A.D.) wrote the Suntaxis, or Almagest, which includes a
cyclopedia of astronomy, containing a summary of knowledge at that
date. We have no evidence beyond his own statement that he was a
practical observer. He theorised on the planetary motions, and held
that the earth is fixed in the centre of the universe. He adopted the
excentric and equant of Hipparchus to explain the unequal motions of
the sun and moon. He adopted the epicycles and deferents which had
been used by Apollonius and others to explain the retrograde motions
of the planets. We, who know that the earth revolves round the sun
once in a year, can understand that the apparent motion of a planet is
only its motion relative to the earth. If, then, we suppose the earth
fixed and the sun to revolve round it once a year, and the planets
each in its own period, it is only necessary to impose upon each of
these an additional _annual_ motion to enable us to represent truly
the apparent motions. This way of looking at the apparent motions
shows why each planet, when nearest to the earth, seems to move for a
time in a retrograde direction. The attempts of Ptolemy and others of
his time to explain the retrograde motion in this way were only
approximate. Let us suppose each planet to have a bar with one end
centred at the earth. If at the other end of the bar one end of a
shorter bar is pivotted, having the planet at its other end, then the
planet is given an annual motion in the secondary circle (the
epicycle), whose centre revolves round the earth on the primary circle
(the _deferent_), at a uniform rate round the excentric. Ptolemy
supposed the centres of the epicycles of Mercury and Venus to be on a
bar passing through the sun, and to be between the earth and the
sun. The centres of the epicycles of Mars, Jupiter, and Saturn were
supposed to be further away than the sun. Mercury and Venus were
supposed to revolve in their epicycles in their own periodic times and
in the deferent round the earth in a year. The major planets were
supposed to revolve in the deferent round the earth in their own
periodic times, and in their epicycles once in a year.

It did not occur to Ptolemy to place the centres of the epicycles of
Mercury and Venus at the sun, and to extend the same system to the
major planets. Something of this sort had been proposed by the
Egyptians (we are told by Cicero and others), and was accepted by
Tycho Brahe; and was as true a representation of the relative motions
in the solar system as when we suppose the sun to be fixed and the
earth to revolve.

The cumbrous system advocated by Ptolemy answered its purpose,
enabling him to predict astronomical events approximately. He improved
the lunar theory considerably, and discovered minor inequalities which
could be allowed for by the addition of new epicycles. We may look
upon these epicycles of Apollonius, and the excentric of Hipparchus,
as the responses of these astronomers to the demand of Plato for
uniform circular motions. Their use became more and more confirmed,
until the seventeenth century, when the accurate observations of Tycho
Brahe enabled Kepler to abolish these purely geometrical makeshifts,
and to substitute a system in which the sun became physically its
controller.

FOOTNOTES:

[1] _Phil. Mag_., vol. xxiv., pp. 481-4.

[2]

Plaeiadas t' esoronte kai ophe duonta bootaen
'Arkton th' aen kai amaxan epiklaesin kaleousin,
'Ae t' autou strephetai kai t' Oriona dokeuei,
Oin d'ammoros esti loetron Okeanoio.

"The Pleiades and Bootes that setteth late, and the Bear,
which they likewise call the Wain, which turneth ever in one
place, and keepeth watch upon Orion, and alone hath no part in
the baths of the ocean."

[3] See Pearson in the Camb. Phil. Soc. Proc., vol. iv., pt. ii., p.
93, on whose authority the above statements are made.

[4] See p. 6 for definition.

4. THE REIGN OF EPICYCLES--FROM PTOLEMY TO COPERNICUS.

After Ptolemy had published his book there seemed to be nothing more
to do for the solar system except to go on observing and finding more
and more accurate values for the constants involved--viz., the periods
of revolution, the diameter of the deferent,[1] and its ratio to that
of the epicycle,[2] the distance of the excentric[3] from the centre
of the deferent, and the position of the line of apses,[4] besides the
inclination and position of the plane of the planet's orbit. The only
object ever aimed at in those days was to prepare tables for
predicting the places of the planets. It was not a mechanical problem;
there was no notion of a governing law of forces.

From this time onwards all interest in astronomy seemed, in Europe at
least, to sink to a low ebb. When the Caliph Omar, in the middle of
the seventh century, burnt the library of Alexandria, which had been
the centre of intellectual progress, that centre migrated to Baghdad,
and the Arabs became the leaders of science and philosophy. In
astronomy they made careful observations. In the middle of the ninth
century Albategnius, a Syrian prince, improved the value of
excentricity of the sun's orbit, observed the motion of the moon's
apse, and thought he detected a smaller progression of the sun's
apse. His tables were much more accurate than Ptolemy's. Abul Wefa, in
the tenth century, seems to have discovered the moon's "variation."
Meanwhile the Moors were leaders of science in the west, and Arzachel
of Toledo improved the solar tables very much. Ulugh Begh, grandson of
the great Tamerlane the Tartar, built a fine observatory at Samarcand
in the fifteenth century, and made a great catalogue of stars, the
first since the time of Hipparchus.

At the close of the fifteenth century King Alphonso of Spain employed
computers to produce the Alphonsine Tables (1488 A.D.), Purbach
translated Ptolemy's book, and observations were carried out in
Germany by Muller, known as Regiomontanus, and Waltherus.

Nicolai Copernicus, a Sclav, was born in 1473 at Thorn, in Polish
Prussia. He studied at Cracow and in Italy. He was a priest, and
settled at Frauenberg. He did not undertake continuous observations,
but devoted himself to simplifying the planetary systems and devising
means for more accurately predicting the positions of the sun, moon,
and planets. He had no idea of framing a solar system on a dynamical
basis. His great object was to increase the accuracy of the
calculations and the tables. The results of his cogitations were
printed just before his death in an interesting book, _De
Revolutionibus Orbium Celestium_. It is only by careful reading of
this book that the true position of Copernicus can be realised. He
noticed that Nicetas and others had ascribed the apparent diurnal
rotation of the heavens to a real daily rotation of the earth about
its axis, in the opposite direction to the apparent motion of the
stars. Also in the writings of Martianus Capella he learnt that the
Egyptians had supposed Mercury and Venus to revolve round the sun, and
to be carried with him in his annual motion round the earth. He
noticed that the same supposition, if extended to Mars, Jupiter, and
Saturn, would explain easily why they, and especially Mars, seem so
much brighter in opposition. For Mars would then be a great deal
nearer to the earth than at other times. It would also explain the
retrograde motion of planets when in opposition.

We must here notice that at this stage Copernicus was actually
confronted with the system accepted later by Tycho Brahe, with the
earth fixed. But he now recalled and accepted the views of Pythagoras
and others, according to which the sun is fixed and the earth
revolves; and it must be noted that, geometrically, there is no
difference of any sort between the Egyptian or Tychonic system and
that of Pythagoras as revived by Copernicus, except that on the latter
theory the stars ought to seem to move when the earth changes its
position--a test which failed completely with the rough means of
observation then available. The radical defect of all solar systems
previous to the time of Kepler (1609 A.D.) was the slavish yielding to
Plato's dictum demanding uniform circular motion for the planets, and
the consequent evolution of the epicycle, which was fatal to any
conception of a dynamical theory.

Copernicus could not sever himself from this obnoxious tradition.[5]
It is true that neither the Pythagorean nor the Egypto-Tychonic system
required epicycles for explaining retrograde motion, as the Ptolemaic
theory did. Furthermore, either system could use the excentric of
Hipparchus to explain the irregular motion known as the equation of
the centre. But Copernicus remarked that he could also use an
epicycle for this purpose, or that he could use both an excentric and
an epicycle for each planet, and so bring theory still closer into
accord with observation. And this he proceeded to do.[6] Moreover,
observers had found irregularities in the moon's motion, due, as we
now know, to the disturbing attraction of the sun. To correct for
these irregularities Copernicus introduced epicycle on epicycle in the
lunar orbit.

This is in its main features the system propounded by Copernicus. But
attention must, to state the case fully, be drawn to two points to be
found in his first and sixth books respectively. The first point
relates to the seasons, and it shows a strange ignorance of the laws
of rotating bodies. To use the words of Delambre,[7] in drawing
attention to the strange conception,

he imagined that the earth, revolving round the sun, ought always to
show to it the same face; the contrary phenomena surprised him: to
explain them he invented a third motion, and added it to the two
real motions (rotation and orbital revolution). By this third motion
the earth, he held, made a revolution on itself and on the poles of
the ecliptic once a year.... Copernicus did not know that motion in
a straight line is the natural motion, and that motion in a curve is
the resultant of several movements. He believed, with Aristotle,
that circular motion was the natural one.

Copernicus made this rotation of the earth's axis about the pole of
the ecliptic retrograde (i.e., opposite to the orbital revolution),
and by making it perform more than one complete revolution in a year,
the added part being 1/26000 of the whole, he was able to include the
precession of the equinoxes in his explanation of the seasons. His
explanation of the seasons is given on leaf 10 of his book (the pages
of this book are not all numbered, only alternate pages, or leaves).

In his sixth book he discusses the inclination of the planetary orbits
to the ecliptic. In regard to this the theory of Copernicus is unique;
and it will be best to explain this in the words of Grant in his great
work.[8] He says:--

Copernicus, as we have already remarked, did not attack the
principle of the epicyclical theory: he merely sought to make it
more simple by placing the centre of the earth's orbit in the centre
of the universe. This was the point to which the motions of the
planets were referred, for the planes of their orbits were made to
pass through it, and their points of least and greatest velocities
were also determined with reference to it. By this arrangement the
sun was situate mathematically near the centre of the planetary
system, but he did not appear to have any physical connexion with
the planets as the centre of their motions.

According to Copernicus' sixth book, the planes of the planetary
orbits do not pass through the sun, and the lines of apses do not pass
through to the sun.

Such was the theory advanced by Copernicus: The earth moves in an
epicycle, on a deferent whose centre is a little distance from the
sun. The planets move in a similar way on epicycles, but their
deferents have no geometrical or physical relation to the sun. The
moon moves on an epicycle centred on a second epicycle, itself centred
on a deferent, excentric to the earth. The earth's axis rotates about
the pole of the ecliptic, making one revolution and a twenty-six
thousandth part of a revolution in the sidereal year, in the opposite
direction to its orbital motion.

In view of this fanciful structure it must be noted, in fairness to
Copernicus, that he repeatedly states that the reader is not obliged
to accept his system as showing the real motions; that it does not
matter whether they be true, even approximately, or not, so long as
they enable us to compute tables from which the places of the planets
among the stars can be predicted.[9] He says that whoever is not
satisfied with this explanation must be contented by being told that
"mathematics are for mathematicians" (Mathematicis mathematica
scribuntur).

At the same time he expresses his conviction over and over again that
the earth is in motion. It is with him a pious belief, just as it was
with Pythagoras and his school and with Aristarchus. "But" (as Dreyer
says in his most interesting book, _Tycho Brahe_) "proofs of the
physical truth of his system Copernicus had given none, and could give
none," any more than Pythagoras or Aristarchus.

There was nothing so startlingly simple in his system as to lead the
cautious astronomer to accept it, as there was in the later Keplerian
system; and the absence of parallax in the stars seemed to condemn his
system, which had no physical basis to recommend it, and no
simplification at all over the Egypto-Tychonic system, to which
Copernicus himself drew attention. It has been necessary to devote
perhaps undue space to the interesting work of Copernicus, because by
a curious chance his name has become so widely known. He has been
spoken of very generally as the founder of the solar system that is
now accepted. This seems unfair, and on reading over what has been
written about him at different times it will be noticed that the
astronomers--those who have evidently read his great book--are very
cautious in the words with which they eulogise him, and refrain from
attributing to him the foundation of our solar system, which is
entirely due to Kepler. It is only the more popular writers who give
the idea that a revolution had been effected when Pythagoras' system
was revived, and when Copernicus supported his view that the earth
moves and is not fixed.

It may be easy to explain the association of the name of Copernicus
with the Keplerian system. But the time has long passed when the
historian can support in any way this popular error, which was started
not by astronomers acquainted with Kepler's work, but by those who
desired to put the Church in the wrong by extolling Copernicus.

Copernicus dreaded much the abuse he expected to receive from
philosophers for opposing the authority of Aristotle, who had declared
that the earth was fixed. So he sought and obtained the support of
the Church, dedicating his great work to Pope Paul III. in a lengthy
explanatory epistle. The Bishop of Cracow set up a memorial tablet in
his honour.

Copernicus was the most refined exponent, and almost the last
representative, of the Epicyclical School. As has been already
stated, his successor, Tycho Brahe, supported the same use of
epicycles and excentrics as Copernicus, though he held the earth to be
fixed. But Tycho Brahe was eminently a practical observer, and took
little part in theory; and his observations formed so essential a
portion of the system of Kepler that it is only fair to include his
name among these who laid the foundations of the solar system which we
accept to-day.

In now taking leave of the system of epicycles let it be remarked that
it has been held up to ridicule more than it deserves. On reading
Airy's account of epicycles, in the beautifully clear language of his
_Six Lectures on Astronomy_, the impression is made that the
jointed bars there spoken of for describing the circles were supposed
to be real. This is no more the case than that the spheres of Eudoxus
and Callippus were supposed to be real. Both were introduced only to
illustrate the mathematical conception upon which the solar,
planetary, and lunar tables were constructed. The epicycles
represented nothing more nor less than the first terms in the Fourier
series, which in the last century has become a basis of such
calculations, both in astronomy and physics generally.

[Illustration: "QUADRANS MURALIS SIVE TICHONICUS." With portrait of
Tycho Brahe, instruments, etc., painted on the wall; showing
assistants using the sight, watching the clock, and recording. (From
the author's copy of the _Astronomiae Instauratae Mechanica._)]

FOOTNOTES:

[1] For definition see p. 22.

[2] _Ibid_.

[3] For definition see p. 18.

[4] For definition see p. 18.

[5] In his great book Copernicus says: "The movement of the heavenly
bodies is uniform, circular, perpetual, or else composed of circular
movements." In this he proclaimed himself a follower of Pythagoras
(see p. 14), as also when he says: "The world is spherical because the
sphere is, of all figures, the most perfect" (Delambre,
_Ast. Mod. Hist_., pp. 86, 87).

[6] Kepler tells us that Tycho Brahe was pleased with this
device, and adapted it to his own system.

[7] _Hist. Ast._, vol. i., p. 354.

[8] _Hist. of Phys. Ast._, p. vii.

[9] "Est enim Astronomi proprium, historiam motuum coelestium
diligenti et artificiosa observatione colligere. Deinde causas
earundem, seu hypotheses, cum veras assequi nulla ratione possit
... Neque enim necesse est, eas hypotheses esse veras, imo ne
verisimiles quidem, sed sufficit hoc usum, si calculum observationibus
congruentem exhibeant."

BOOK II. THE DYNAMICAL PERIOD

5. DISCOVERY OF THE TRUE SOLAR SYSTEM--TYCHO BRAHE--KEPLER.

During the period of the intellectual and aesthetic revival, at the
beginning of the sixteenth century, the "spirit of the age" was
fostered by the invention of printing, by the downfall of the
Byzantine Empire, and the scattering of Greek fugitives, carrying the
treasures of literature through Western Europe, by the works of
Raphael and Michael Angelo, by the Reformation, and by the extension
of the known world through the voyages of Spaniards and Portuguese.
During that period there came to the front the founder of accurate
observational astronomy. Tycho Brahe, a Dane, born in 1546 of noble
parents, was the most distinguished, diligent, and accurate observer
of the heavens since the days of Hipparchus, 1,700 years before.

Tycho was devoted entirely to his science from childhood, and the
opposition of his parents only stimulated him in his efforts to
overcome difficulties. He soon grasped the hopelessness of the old
deductive methods of reasoning, and decided that no theories ought to
be indulged in until preparations had been made by the accumulation of
accurate observations. We may claim for him the title of founder of
the inductive method.

For a complete life of this great man the reader is referred to
Dreyer's _Tycho Brahe_, Edinburgh, 1890, containing a complete
bibliography. The present notice must be limited to noting the work
done, and the qualities of character which enabled him to attain his
scientific aims, and which have been conspicuous in many of his
successors.

He studied in Germany, but King Frederick of Denmark, appreciating his
great talents, invited him to carry out his life's work in that
country. He granted to him the island of Hveen, gave him a pension,
and made him a canon of the Cathedral of Roskilde. On that island
Tycho Brahe built the splendid observatory which he called Uraniborg,
and, later, a second one for his assistants and students, called
Stjerneborg. These he fitted up with the most perfect instruments, and
never lost a chance of adding to his stock of careful observations.[1]

The account of all these instruments and observations, printed at his
own press on the island, was published by Tycho Brahe himself, and the
admirable and numerous engravings bear witness to the excellence of
design and the stability of his instruments.

His mechanical skill was very great, and in his workmanship he was
satisfied with nothing but the best. He recognised the importance of
rigidity in the instruments, and, whereas these had generally been
made of wood, he designed them in metal. His instruments included
armillae like those which had been used in Alexandria, and other
armillae designed by himself--sextants, mural quadrants, large
celestial globes and various instruments for special purposes. He
lived before the days of telescopes and accurate clocks. He invented
the method of sub-dividing the degrees on the arc of an instrument by
transversals somewhat in the way that Pedro Nunez had proposed.

He originated the true system of observation and reduction of
observations, recognising the fact that the best instrument in the
world is not perfect; and with each of his instruments he set to work
to find out the errors of graduation and the errors of mounting, the
necessary correction being applied to each observation.

When he wanted to point his instrument exactly to a star he was
confronted with precisely the same difficulty as is met in gunnery and
rifle-shooting. The sights and the object aimed at cannot be in focus
together, and a great deal depends on the form of sight. Tycho Brahe
invented, and applied to the pointers of his instruments, an
aperture-sight of variable area, like the iris diaphragm used now in
photography. This enabled him to get the best result with stars of
different brightness. The telescope not having been invented, he
could not use a telescopic-sight as we now do in gunnery. This not
only removes the difficulty of focussing, but makes the minimum
visible angle smaller. Helmholtz has defined the minimum angle
measurable with the naked eye as being one minute of arc. In view of
this it is simply marvellous that, when the positions of Tycho's
standard stars are compared with the best modern catalogues, his
probable error in right ascension is only +/- 24", 1, and in declination
only +/- 25", 9.

Clocks of a sort had been made, but Tycho Brahe found them so
unreliable that he seldom used them, and many of his position-measurements
were made by measuring the angular distances from known stars.

Taking into consideration the absence of either a telescope or a
clock, and reading his account of the labour he bestowed upon each
observation, we must all agree that Kepler, who inherited these
observations in MS., was justified, under the conditions then
existing, in declaring that there was no hope of anyone ever improving
upon them.

In the year 1572, on November 11th, Tycho discovered in Cassiopeia a
new star of great brilliance, and continued to observe it until the
end of January, 1573. So incredible to him was such an event that he
refused to believe his own eyes until he got others to confirm what he
saw. He made accurate observations of its distance from the nine
principal stars in Casseiopeia, and proved that it had no measurable
parallax. Later he employed the same method with the comets of 1577,
1580, 1582, 1585, 1590, 1593, and 1596, and proved that they too had
no measurable parallax and must be very distant.

The startling discovery that stars are not necessarily permanent, that
new stars may appear, and possibly that old ones may disappear, had
upon him exactly the same effect that a similar occurrence had upon
Hipparchus 1,700 years before. He felt it his duty to catalogue all
the principal stars, so that there should be no mistake in the
future. During the construction of his catalogue of 1,000 stars he
prepared and used accurate tables of refraction deduced from his own
observations. Thus he eliminated (so far as naked eye observations
required) the effect of atmospheric refraction which makes the
altitude of a star seem greater than it really is.

Tycho Brahe was able to correct the lunar theory by his observations.
Copernicus had introduced two epicycles on the lunar orbit in the hope
of obtaining a better accordance between theory and observation; and
he was not too ambitious, as his desire was to get the tables accurate
to ten minutes. Tycho Brahe found that the tables of Copernicus were
in error as much as two degrees. He re-discovered the inequality
called "variation" by observing the moon in all phases--a thing which
had not been attended to. [It is remarkable that in the nineteenth
century Sir George Airy established an altazimuth at Greenwich
Observatory with this special object, to get observations of the moon
in all phases.] He also discovered other lunar equalities, and wanted
to add another epicycle to the moon's orbit, but he feared that these
would soon become unmanageable if further observations showed more new
inequalities.

But, as it turned out, the most fruitful work of Tycho Brahe was on
the motions of the planets, and especially of the planet Mars, for it
was by an examination of these results that Kepler was led to the
discovery of his immortal laws.

After the death of King Frederick the observatories of Tycho Brahe
were not supported. The gigantic power and industry displayed by this
determined man were accompanied, as often happens, by an overbearing
manner, intolerant of obstacles. This led to friction, and eventually
the observatories were dismantled, and Tycho Brahe was received by the
Emperor Rudolph II., who placed a house in Prague at his disposal.
Here he worked for a few years, with Kepler as one of his assistants,
and he died in the year 1601.

It is an interesting fact that Tycho Brahe had a firm conviction that
mundane events could be predicted by astrology, and that this belief
was supported by his own predictions.

It has already been stated that Tycho Brahe maintained that
observation must precede theory. He did not accept the Copernican
theory that the earth moves, but for a working hypothesis he used a
modification of an old Egyptian theory, mathematically identical with
that of Copernicus, but not involving a stellar parallax. He says
(_De Mundi_, etc.) that

the Ptolemean system was too complicated, and the new one which that
great man Copernicus had proposed, following in the footsteps of
Aristarchus of Samos, though there was nothing in it contrary to
mathematical principles, was in opposition to those of physics, as
the heavy and sluggish earth is unfit to move, and the system is
even opposed to the authority of Scripture. The absence of annual
parallax further involves an incredible distance between the
outermost planet and the fixed stars.

We are bound to admit that in the circumstances of the case, so long
as there was no question of dynamical forces connecting the members of
the solar system, his reasoning, as we should expect from such a man,
is practical and sound. It is not surprising, then, that astronomers
generally did not readily accept the views of Copernicus, that Luther
(Luther's _Tischreden_, pp. 22, 60) derided him in his usual pithy
manner, that Melancthon (_Initia doctrinae physicae_) said that
Scripture, and also science, are against the earth's motion; and that
the men of science whose opinion was asked for by the cardinals (who
wished to know whether Galileo was right or wrong) looked upon
Copernicus as a weaver of fanciful theories.

Johann Kepler is the name of the man whose place, as is generally
agreed, would have been the most difficult to fill among all those who
have contributed to the advance of astronomical knowledge. He was born
at Wiel, in the Duchy of Wurtemberg, in 1571. He held an appointment
at Gratz, in Styria, and went to join Tycho Brahe in Prague, and to
assist in reducing his observations. These came into his possession
when Tycho Brahe died, the Emperor Rudolph entrusting to him the
preparation of new tables (called the Rudolphine tables) founded on
the new and accurate observations. He had the most profound respect
for the knowledge, skill, determination, and perseverance of the man
who had reaped such a harvest of most accurate data; and though Tycho
hardly recognised the transcendent genius of the man who was working
as his assistant, and although there were disagreements between them,
Kepler held to his post, sustained by the conviction that, with these
observations to test any theory, he would be in a position to settle
for ever the problem of the solar system.

[Illustration: PORTRAIT OF JOHANNES KEPLER. By F. Wanderer, from
Reitlinger's "Johannes Kepler" (original in Strassburg).]

It has seemed to many that Plato's demand for uniform circular motion
(linear or angular) was responsible for a loss to astronomy of good
work during fifteen hundred years, for a hundred ill-considered
speculative cosmogonies, for dissatisfaction, amounting to disgust,
with these _a priori_ guesses, and for the relegation of the
science to less intellectual races than Greeks and other Europeans.
Nobody seemed to dare to depart from this fetish of uniform angular
motion and circular orbits until the insight, boldness, and
independence of Johann Kepler opened up a new world of thought and of
intellectual delight.

While at work on the Rudolphine tables he used the old epicycles and
deferents and excentrics, but he could not make theory agree with
observation. His instincts told him that these apologists for uniform
motion were a fraud; and he proved it to himself by trying every
possible variation of the elements and finding them fail. The number
of hypotheses which he examined and rejected was almost incredible
(for example, that the planets turn round centres at a little distance
from the sun, that the epicycles have centres at a little distance
from the deferent, and so on). He says that, after using all these
devices to make theory agree with Tycho's observations, he still found
errors amounting to eight minutes of a degree. Then he said boldly
that it was impossible that so good an observer as Tycho could have
made a mistake of eight minutes, and added: "Out of these eight
minutes we will construct a new theory that will explain the motions
of all the planets." And he did it, with elliptic orbits having the
sun in a focus of each.[2]

It is often difficult to define the boundaries between fancies,
imagination, hypothesis, and sound theory. This extraordinary genius
was a master in all these modes of attacking a problem. His analogy
between the spaces occupied by the five regular solids and the
distances of the planets from the sun, which filled him with so much
delight, was a display of pure fancy. His demonstration of the three
fundamental laws of planetary motion was the most strict and complete
theory that had ever been attempted.

It has been often suggested that the revival by Copernicus of the
notion of a moving earth was a help to Kepler. No one who reads
Kepler's great book could hold such an opinion for a moment. In fact,
the excellence of Copernicus's book helped to prolong the life of the
epicyclical theories in opposition to Kepler's teaching.

All of the best theories were compared by him with observation. These
were the Ptolemaic, the Copernican, and the Tychonic. The two latter
placed all of the planetary orbits concentric with one another, the
sun being placed a little away from their common centre, and having no
apparent relation to them, and being actually outside the planes in
which they move. Kepler's first great discovery was that the planes
of all the orbits pass through the sun; his second was that the line
of apses of each planet passes through the sun; both were
contradictory to the Copernican theory.

He proceeds cautiously with his propositions until he arrives at his
great laws, and he concludes his book by comparing observations of
Mars, of all dates, with his theory.

His first law states that the planets describe ellipses with the sun
at a focus of each ellipse.

His second law (a far more difficult one to prove) states that a line
drawn from a planet to the sun sweeps over equal areas in equal
times. These two laws were published in his great work, _Astronomia
Nova, sen. Physica Coelestis tradita commentariis de Motibus Stelloe;
Martis_, Prague, 1609.

It took him nine years more[3] to discover his third law, that the
squares of the periodic times are proportional to the cubes of the
mean distances from the sun.

These three laws contain implicitly the law of universal
gravitation. They are simply an alternative way of expressing that law
in dealing with planets, not particles. Only, the power of the
greatest human intellect is so utterly feeble that the meaning of the
words in Kepler's three laws could not be understood until expounded
by the logic of Newton's dynamics.

The joy with which Kepler contemplated the final demonstration of
these laws, the evolution of which had occupied twenty years, can
hardly be imagined by us. He has given some idea of it in a passage
in his work on _Harmonics_, which is not now quoted, only lest
someone might say it was egotistical--a term which is simply grotesque
when applied to such a man with such a life's work accomplished.

The whole book, _Astronomia Nova_, is a pleasure to read; the
mass of observations that are used, and the ingenuity of the
propositions, contrast strongly with the loose and imperfectly
supported explanations of all his predecessors; and the indulgent
reader will excuse the devotion of a few lines to an example of the
ingenuity and beauty of his methods.

It may seem a hopeless task to find out the true paths of Mars and the
earth (at that time when their shape even was not known) from the
observations giving only the relative direction from night to
night. Now, Kepler had twenty years of observations of Mars to deal
with. This enabled him to use a new method, to find the earth's
orbit. Observe the date at any time when Mars is in opposition. The
earth's position E at that date gives the longitude of Mars M. His
period is 687 days. Now choose dates before and after the principal
date at intervals of 687 days and its multiples. Mars is in each case
in the same position. Now for any date when Mars is at M and the earth
at E3 the date of the year gives the angle E3SM. And the
observation of Tycho gives the direction of Mars compared with the
sun, SE3M. So all the angles of the triangle SEM in any of these
positions of E are known, and also the ratios of SE1, SE2, SE3,
SE4 to SM and to each other.

For the orbit of Mars observations were chosen at intervals of a year,
when the earth was always in the same place.

[Illustration]

But Kepler saw much farther than the geometrical facts. He realised
that the orbits are followed owing to a force directed to the sun; and
he guessed that this is the same force as the gravity that makes a
stone fall. He saw the difficulty of gravitation acting through the
void space. He compared universal gravitation to magnetism, and
speaks of the work of Gilbert of Colchester. (Gilbert's book, _De
Mundo Nostro Sublunari, Philosophia Nova_, Amstelodami, 1651,
containing similar views, was published forty-eight years after
Gilbert's death, and forty-two years after Kepler's book and
reference. His book _De Magnete_ was published in 1600.)

A few of Kepler's views on gravitation, extracted from the
Introduction to his _Astronomia Nova_, may now be mentioned:--

1. Every body at rest remains at rest if outside the attractive power
of other bodies.

2. Gravity is a property of masses mutually attracting in such manner
that the earth attracts a stone much more than a stone attracts the
earth.

3. Bodies are attracted to the earth's centre, not because it is the
centre of the universe, but because it is the centre of the attracting
particles of the earth.

4. If the earth be not round (but spheroidal?), then bodies at
different latitudes will not be attracted to its centre, but to
different points in the neighbourhood of that centre.

5. If the earth and moon were not retained in their orbits by vital
force (_aut alia aligua aequipollenti_), the earth and moon would come
together.

6. If the earth were to cease to attract its waters, the oceans would
all rise and flow to the moon.

7. He attributes the tides to lunar attraction. Kepler had been
appointed Imperial Astronomer with a handsome salary (on paper), a
fraction of which was doled out to him very irregularly. He was led to
miserable makeshifts to earn enough to keep his family from
starvation; and proceeded to Ratisbon in 1630 to represent his claims
to the Diet. He arrived worn out and debilitated; he failed in his
appeal, and died from fever, contracted under, and fed upon,
disappointment and exhaustion. Those were not the days when men could
adopt as a profession the "research of endowment."

Before taking leave of Kepler, who was by no means a man of one idea,
it ought to be here recorded that he was the first to suggest that a
telescope made with both lenses convex (not a Galilean telescope) can
have cross wires in the focus, for use as a pointer to fix accurately
the positions of stars. An Englishman, Gascoigne, was the first to use
this in practice.

From the all too brief epitome here given of Kepler's greatest book,
it must be obvious that he had at that time some inkling of the
meaning of his laws--universal gravitation. From that moment the idea
of universal gravitation was in the air, and hints and guesses were
thrown out by many; and in time the law of gravitation would doubtless
have been discovered, though probably not by the work of one man, even
if Newton had not lived. But, if Kepler had not lived, who else could
have discovered his laws?

FOOTNOTES:

[1] When the writer visited M. D'Arrest, the astronomer, at
Copenhagen, in 1872, he was presented by D'Arrest with one of several
bricks collected from the ruins of Uraniborg. This was one of his most
cherished possessions until, on returning home after a prolonged
absence on astronomical work, he found that his treasure had been
tidied away from his study.

[2] An ellipse is one of the plane, sections of a cone. It is an oval
curve, which may be drawn by fixing two pins in a sheet of paper at S
and H, fastening a string, SPH, to the two pins, and stretching it
with a pencil point at P, and moving the pencil point, while the
string is kept taut, to trace the oval ellipse, APB. S and H are the
_foci_. Kepler found the sun to be in one focus, say S. AB is the
_major axis_. DE is the _minor axis_. C is the _centre_. The direction
of AB is the _line of apses_. The ratio of CS to CA is the
_excentricity_. The position of the planet at A is the _perihelion_
(nearest to the sun). The position of the planet at B is the
_aphelion_ (farthest from the sun). The angle ASP is the _anomaly_
when the planet is at P. CA or a line drawn from S to D is the _mean
distance_ of the planet from the sun.

[Illustration]

[3] The ruled logarithmic paper we now use was not then to be had by
going into a stationer's shop. Else he would have accomplished this in
five minutes.

6. GALILEO AND THE TELESCOPE--NOTIONS OF GRAVITY BY HORROCKS, ETC.

It is now necessary to leave the subject of dynamical astronomy for a
short time in order to give some account of work in a different
direction originated by a contemporary of Kepler's, his senior in fact
by seven years. Galileo Galilei was born at Pisa in 1564. The most
scientific part of his work dealt with terrestrial dynamics; but one
of those fortunate chances which happen only to really great men put
him in the way of originating a new branch of astronomy.

The laws of motion had not been correctly defined. The only man of
Galileo's time who seems to have worked successfully in the same
direction as himself was that Admirable Crichton of the Italians,
Leonardo da Vinci. Galileo cleared the ground. It had always been
noticed that things tend to come to rest; a ball rolled on the ground,
a boat moved on the water, a shot fired in the air. Galileo realised
that in all of these cases a resisting force acts to stop the motion,
and he was the first to arrive at the not very obvious law that the
motion of a body will never stop, nor vary its speed, nor change its
direction, except by the action of some force.

It is not very obvious that a light body and a heavy one fall at the
same speed (except for the resistance of the air). Galileo proved this
on paper, but to convince the world he had to experiment from the
leaning tower of Pisa.

At an early age he discovered the principle of isochronism of the
pendulum, which, in the hands of Huyghens in the middle of the
seventeenth century, led to the invention of the pendulum clock,
perhaps the most valuable astronomical instrument ever produced.

These and other discoveries in dynamics may seem very obvious now; but
it is often the most every-day matters which have been found to elude
the inquiries of ordinary minds, and it required a high order of
intellect to unravel the truth and discard the stupid maxims scattered
through the works of Aristotle and accepted on his authority. A blind
worship of scientific authorities has often delayed the progress of
human knowledge, just as too much "instruction" of a youth often ruins
his "education." Grant, in his history of Physical Astronomy, has well
said that "the sagacity and skill which Galileo displays in resolving
the phenomena of motion into their constituent elements, and hence
deriving the original principles involved in them, will ever assure to
him a distinguished place among those who have extended the domains of
science."

But it was work of a different kind that established Galileo's popular
reputation. In 1609 Galileo heard that a Dutch spectacle-maker had
combined a pair of lenses so as to magnify distant objects. Working on
this hint, he solved the same problem, first on paper and then in
practice. So he came to make one of the first telescopes ever used in
astronomy. No sooner had he turned it on the heavenly bodies than he
was rewarded by such a shower of startling discoveries as forthwith
made his name the best known in Europe. He found curious irregular
black spots on the sun, revolving round it in twenty-seven days; hills
and valleys on the moon; the planets showing discs of sensible size,
not points like the fixed stars; Venus showing phases according to her
position in relation to the sun; Jupiter accompanied by four moons;
Saturn with appendages that he could not explain, but unlike the other
planets; the Milky Way composed of a multitude of separate stars.

His fame flew over Europe like magic, and his discoveries were much
discussed--and there were many who refused to believe. Cosmo de Medici
induced him to migrate to Florence to carry on his observations. He
was received by Paul V., the Pope, at Rome, to whom he explained his
discoveries.

He thought that these discoveries proved the truth of the Copernican
theory of the Earth's motion; and he urged this view on friends and
foes alike. Although in frequent correspondence with Kepler, he never
alluded to the New Astronomy, and wrote to him extolling the virtue of
epicycles. He loved to argue, never shirked an encounter with any
number of disputants, and laughed as he broke down their arguments.

Through some strange course of events, not easy to follow, the
Copernican theory, whose birth was welcomed by the Church, had now
been taken up by certain anti-clerical agitators, and was opposed by
the cardinals as well as by the dignitaries of the Reformed
Church. Galileo--a good Catholic--got mixed up in these discussions,
although on excellent terms with the Pope and his entourage. At last
it came about that Galileo was summoned to appear at Rome, where he
was charged with holding and teaching heretical opinions about the
movement of the earth; and he then solemnly abjured these
opinions. There has been much exaggeration and misstatement about his
trial and punishment, and for a long time there was a great deal of
bitterness shown on both sides. But the general verdict of the present
day seems to be that, although Galileo himself was treated with
consideration, the hostility of the Church to the views of Copernicus
placed it in opposition also to the true Keplerian system, and this
led to unprofitable controversies. From the time of Galileo onwards,
for some time, opponents of religion included the theory of the
Earth's motion in their disputations, not so much for the love, or
knowledge, of astronomy, as for the pleasure of putting the Church in
the wrong. This created a great deal of bitterness and intolerance on
both sides. Among the sufferers was Giordano Bruno, a learned
speculative philosopher, who was condemned to be burnt at the stake.

Galileo died on Christmas Day, 1642--the day of Newton's birth. The
further consideration of the grand field of discovery opened out by
Galileo with his telescopes must be now postponed, to avoid
discontinuity in the history of the intellectual development of this
period, which lay in the direction of dynamical, or physical,
astronomy.

Until the time of Kepler no one seems to have conceived the idea of
universal physical forces controlling terrestrial phenomena, and
equally applicable to the heavenly bodies. The grand discovery by
Kepler of the true relationship of the Sun to the Planets, and the
telescopic discoveries of Galileo and of those who followed him,
spread a spirit of inquiry and philosophic thought throughout Europe,
and once more did astronomy rise in estimation; and the irresistible
logic of its mathematical process of reasoning soon placed it in the
position it has ever since occupied as the foremost of the exact
sciences.

The practical application of this process of reasoning was enormously
facilitated by the invention of logarithms by Napier. He was born at
Merchistoun, near Edinburgh, in 1550, and died in 1617. By this system
the tedious arithmetical operations necessary in astronomical
calculations, especially those dealing with the trigonometrical
functions of angles, were so much simplified that Laplace declared
that by this invention the life-work of an astronomer was doubled.

Jeremiah Horrocks (born 1619, died 1641) was an ardent admirer of
Tycho Brahe and Kepler, and was able to improve the Rudolphine tables
so much that he foretold a transit of Venus, in 1639, which these
tables failed to indicate, and was the only observer of it. His life
was short, but he accomplished a great deal, and rightly ascribed the
lunar inequality called _evection_ to variations in the value of
the eccentricity and in the direction of the line of apses, at the
same time correctly assigning _the disturbing force of the Sun_
as the cause. He discovered the errors in Jupiter's calculated place,
due to what we now know as the long inequality of Jupiter and Saturn,
and measured with considerable accuracy the acceleration at that date
of Jupiter's mean motion, and indicated the retardation of Saturn's
mean motion.

Horrocks' investigations, so far as they could be collected, were
published posthumously in 1672, and seldom, if ever, has a man who
lived only twenty-two years originated so much scientific knowledge.

At this period British science received a lasting impetus by the wise
initiation of a much-abused man, Charles II., who founded the Royal
Society of London, and also the Royal Observatory of Greeenwich, where
he established Flamsteed as first Astronomer Royal, especially for
lunar and stellar observations likely to be useful for navigation. At
the same time the French Academy and the Paris Observatory were
founded. All this within fourteen years, 1662-1675.

Meanwhile gravitation in general terms was being discussed by Hooke,
Wren, Halley, and many others. All of these men felt a repugnance to
accept the idea of a force acting across the empty void of space.
Descartes (1596-1650) proposed an ethereal medium whirling round the
sun with the planets, and having local whirls revolving with the
satellites. As Delambre and Grant have said, this fiction only
retarded the progress of pure science. It had no sort of relation to
the more modern, but equally misleading, "nebular hypothesis." While
many were talking and guessing, a giant mind was needed at this stage
to make things clear.

7. SIR ISAAC NEWTON--LAW OF UNIVERSAL GRAVITATION.

We now reach the period which is the culminating point of interest in
the history of dynamical astronomy. Isaac Newton was born in
1642. Pemberton states that Newton, having quitted Cambridge to avoid
the plague, was residing at Wolsthorpe, in Lincolnshire, where he had
been born; that he was sitting one day in the garden, reflecting upon
the force which prevents a planet from flying off at a tangent and
which draws it to the sun, and upon the force which draws the moon to
the earth; and that he saw in the case of the planets that the sun's
force must clearly be unequal at different distances, for the pull out
of the tangential line in a minute is less for Jupiter than for
Mars. He then saw that the pull of the earth on the moon would be less
than for a nearer object. It is said that while thus meditating he saw
an apple fall from a tree to the ground, and that this fact suggested
the questions: Is the force that pulled that apple from the tree the
same as the force which draws the moon to the earth? Does the
attraction for both of them follow the same law as to distance as is
given by the planetary motions round the sun? It has been stated that
in this way the first conception of universal gravitation arose.[1]

Quite the most important event in the whole history of physical
astronomy was the publication, in 1687, of Newton's _Principia
(Philosophiae Naturalis Principia Mathematica)_. In this great work
Newton started from the beginning of things, the laws of motion, and
carried his argument, step by step, into every branch of physical
astronomy; giving the physical meaning of Kepler's three laws, and
explaining, or indicating the explanation of, all the known heavenly
motions and their irregularities; showing that all of these were
included in his simple statement about the law of universal
gravitation; and proceeding to deduce from that law new irregularities
in the motions of the moon which had never been noticed, and to
discover the oblate figure of the earth and the cause of the
tides. These investigations occupied the best part of his life; but he
wrote the whole of his great book in fifteen months.

Having developed and enunciated the true laws of motion, he was able
to show that Kepler's second law (that equal areas are described by
the line from the planet to the sun in equal times) was only another
way of saying that the centripetal force on a planet is always
directed to the sun. Also that Kepler's first law (elliptic orbits
with the sun in one focus) was only another way of saying that the
force urging a planet to the sun varies inversely as the square of the
distance. Also (if these two be granted) it follows that Kepler's
third law is only another way of saying that the sun's force on
different planets (besides depending as above on distance) is
proportional to their masses.

Having further proved the, for that day, wonderful proposition that,
with the law of inverse squares, the attraction by the separate
particles of a sphere of uniform density (or one composed of
concentric spherical shells, each of uniform density) acts as if the
whole mass were collected at the centre, he was able to express the
meaning of Kepler's laws in propositions which have been summarised as
follows:--

The law of universal gravitation.--_Every particle of matter in the
universe attracts every other particle with a force varying inversely
as the square of the distance between them, and directly as the
product of the masses of the two particles_.[2]

But Newton did not commit himself to the law until he had answered
that question about the apple; and the above proposition now enabled
him to deal with the Moon and the apple. Gravity makes a stone fall
16.1 feet in a second. The moon is 60 times farther from the earth's
centre than the stone, so it ought to be drawn out of a straight
course through 16.1 feet in a minute. Newton found the distance
through which she is actually drawn as a fraction of the earth's
diameter. But when he first examined this matter he proceeded to use
a wrong diameter for the earth, and he found a serious discrepancy.
This, for a time, seemed to condemn his theory, and regretfully he
laid that part of his work aside. Fortunately, before Newton wrote the
_Principia_ the French astronomer Picard made a new and correct
measure of an arc of the meridian, from which he obtained an accurate
value of the earth's diameter. Newton applied this value, and found,
to his great joy, that when the distance of the moon is 60 times the
radius of the earth she is attracted out of the straight course 16.1
feet per minute, and that the force acting on a stone or an apple
follows the same law as the force acting upon the heavenly bodies.[3]

The universality claimed for the law--if not by Newton, at least by
his commentators--was bold, and warranted only by the large number of
cases in which Newton had found it to apply. Its universality has been
under test ever since, and so far it has stood the test. There has
often been a suspicion of a doubt, when some inequality of motion in
the heavenly bodies has, for a time, foiled the astronomers in their
attempts to explain it. But improved mathematical methods have always
succeeded in the end, and so the seeming doubt has been converted into
a surer conviction of the universality of the law.

Having once established the law, Newton proceeded to trace some of its
consequences. He saw that the figure of the earth depends partly on
the mutual gravitation of its parts, and partly on the centrifugal
tendency due to the earth's rotation, and that these should cause a
flattening of the poles. He invented a mathematical method which he
used for computing the ratio of the polar to the equatorial diameter.

He then noticed that the consequent bulging of matter at the equator
would be attracted by the moon unequally, the nearest parts being most
attracted; and so the moon would tend to tilt the earth when in some
parts of her orbit; and the sun would do this to a less extent,
because of its great distance. Then he proved that the effect ought to
be a rotation of the earth's axis over a conical surface in space,
exactly as the axis of a top describes a cone, if the top has a sharp
point, and is set spinning and displaced from the vertical. He
actually calculated the amount; and so he explained the cause of the
precession of the equinoxes discovered by Hipparchus about 150 B.C.

One of his grandest discoveries was a method of weighing the heavenly
bodies by their action on each other. By means of this principle he
was able to compare the mass of the sun with the masses of those
planets that have moons, and also to compare the mass of our moon with
the mass of the earth.

Thus Newton, after having established his great principle, devoted his
splendid intellect to the calculation of its consequences. He proved
that if a body be projected with any velocity in free space, subject
only to a central force, varying inversely as the square of the
distance, the body must revolve in a curve which may be any one of the
sections of a cone--a circle, ellipse, parabola, or hyperbola; and he
found that those comets of which he had observations move in parabolae
round the Sun, and are thus subject to the universal law.

Newton realised that, while planets and satellites are chiefly
controlled by the central body about which they revolve, the new law
must involve irregularities, due to their mutual action--such, in
fact, as Horrocks had indicated. He determined to put this to a test
in the case of the moon, and to calculate the sun's effect, from its
mass compared with that of the earth, and from its distance. He proved
that the average effect upon the plane of the orbit would be to cause
the line in which it cuts the plane of the ecliptic (i.e., the line of
nodes) to revolve in the ecliptic once in about nineteen years. This
had been a known fact from the earliest ages. He also concluded that
the line of apses would revolve in the plane of the lunar orbit also
in about nineteen years; but the observed period is only ten
years. For a long time this was the one weak point in the Newtonian
theory. It was not till 1747 that Clairaut reconciled this with the
theory, and showed why Newton's calculation was not exact.

Newton proceeded to explain the other inequalities recognised by Tycho
Brahe and older observers, and to calculate their maximum amounts as
indicated by his theory. He further discovered from his calculations
two new inequalities, one of the apogee, the other of the nodes, and
assigned the maximum value. Grant has shown the values of some of
these as given by observation in the tables of Meyer and more modern
tables, and has compared them with the values assigned by Newton from
his theory; and the comparison is very remarkable.

Newton. Modern Tables.
degrees ' " degrees ' "
Mean monthly motion of Apses 1.31.28 3.4.0
Mean annual motion of nodes 19.18.1,23 19.21.22,50
Mean value of "variation" 36.10 35.47
Annual equation 11.51 11.14
Inequality of mean motion of apogee 19.43 22.17
Inequality of mean motion of nodes 9.24 9.0

The only serious discrepancy is the first, which has been already
mentioned. Considering that some of these perturbations had never been
discovered, that the cause of none of them had ever been known, and
that he exhibited his results, if he did not also make the
discoveries, by the synthetic methods of geometry, it is simply
marvellous that he reached to such a degree of accuracy. He invented
the infinitesimal calculus which is more suited for such calculations,
but had he expressed his results in that language he would have been
unintelligible to many.

Newton's method of calculating the precession of the equinoxes,
already referred to, is as beautiful as anything in the _Principia_.
He had already proved the regression of the nodes of a satellite
moving in an orbit inclined to the ecliptic. He now said that the
nodes of a ring of satellites revolving round the earth's equator
would consequently all regress. And if joined into a solid ring its
node would regress; and it would do so, only more slowly, if
encumbered by the spherical part of the earth's mass. Therefore the
axis of the equatorial belt of the earth must revolve round the pole
of the ecliptic. Then he set to work and found the amount due to the
moon and that due to the sun, and so he solved the mystery of 2,000
years.

When Newton applied his law of gravitation to an explanation of the
tides he started a new field for the application of mathematics to
physical problems; and there can be little doubt that, if he could
have been furnished with complete tidal observations from different
parts of the world, his extraordinary powers of analysis would have
enabled him to reach a satisfactory theory. He certainly opened up
many mines full of intellectual gems; and his successors have never
ceased in their explorations. This has led to improved mathematical
methods, which, combined with the greater accuracy of observation,
have rendered physical astronomy of to-day the most exact of the
sciences.

Laplace only expressed the universal opinion of posterity when he said
that to the _Principia_ is assured "a pre-eminence above all the
other productions of the human intellect."

The name of Flamsteed, First Astronomer Royal, must here be mentioned
as having supplied Newton with the accurate data required for
completing the theory.

The name of Edmund Halley, Second Astronomer Royal, must ever be held
in repute, not only for his own discoveries, but for the part he
played in urging Newton to commit to writing, and present to the Royal
Society, the results of his investigations. But for his friendly
insistence it is possible that the _Principia_ would never have
been written; and but for his generosity in supplying the means the
Royal Society could not have published the book.

[Illustration: DEATH MASK OF SIR ISAAC NEWTON.
Photographed specially for this work from the original, by kind
permission of the Royal Society, London.]

Sir Isaac Newton died in 1727, at the age of eighty-five. His body
lay in state in the Jerusalem Chamber, and was buried in Westminster
Abbey.

FOOTNOTES:

[1] The writer inherited from his father (Professor J. D. Forbes) a
small box containing a bit of wood and a slip of paper, which had been
presented to him by Sir David Brewster. On the paper Sir David had
written these words: "If there be any truth in the story that Newton
was led to the theory of gravitation by the fall of an apple, this bit
of wood is probably a piece of the apple tree from which Newton saw
the apple fall. When I was on a pilgrimage to the house in which
Newton was born, I cut it off an ancient apple tree growing in his
garden." When lecturing in Glasgow, about 1875, the writer showed it
to his audience. The next morning, when removing his property from the
lecture table, he found that his precious relic had been stolen. It
would be interesting to know who has got it now!

[2] It must be noted that these words, in which the laws of
gravitation are always summarised in histories and text-books, do not
appear in the _Principia_; but, though they must have been composed by
some early commentator, it does not appear that their origin has been
traced. Nor does it appear that Newton ever extended the law beyond
the Solar System, and probably his caution would have led him to avoid
any statement of the kind until it should be proved.

With this exception the above statement of the law of universal
gravitation contains nothing that is not to be found in the
_Principia_; and the nearest approach to that statement occurs in the
Seventh Proposition of Book III.:--

Prop.: That gravitation occurs in all bodies, and that it is
proportional to the quantity of matter in each.

Cor. I.: The total attraction of gravitation on a planet arises, and
is composed, out of the attraction on the separate parts.

Cor. II.: The attraction on separate equal particles of a body is
reciprocally as the square of the distance from the particles.

[3] It is said that, when working out this final result, the
probability of its confirming that part of his theory which he had
reluctantly abandoned years before excited him so keenly that he was
forced to hand over his calculations to a friend, to be completed by
him.

8. NEWTON'S SUCCESSORS--HALLEY, EULER, LAGRANGE, LAPLACE, ETC.

Edmund Halley succeeded Flamsteed as Second Astronomer Royal in
1721. Although he did not contribute directly to the mathematical
proofs of Newton's theory, yet his name is closely associated with
some of its greatest successes.

He was the first to detect the acceleration of the moon's mean
motion. Hipparchus, having compared his own observations with those of
more ancient astronomers, supplied an accurate value of the moon's
mean motion in his time. Halley similarly deduced a value for modern
times, and found it sensibly greater. He announced this in 1693, but
it was not until 1749 that Dunthorne used modern lunar tables to
compute a lunar eclipse observed in Babylon 721 B.C., another at
Alexandria 201 B.C., a solar eclipse observed by Theon 360 A.D., and
two later ones up to the tenth century. He found that to explain
these eclipses Halley's suggestion must be adopted, the acceleration
being 10" in one century. In 1757 Lalande again fixed it at 10."

The Paris Academy, in 1770, offered their prize for an investigation
to see if this could be explained by the theory of gravitation. Euler
won the prize, but failed to explain the effect, and said: "It appears
to be established by indisputable evidence that the secular inequality
of the moon's mean motion cannot be produced by the forces of
gravitation."

The same subject was again proposed for a prize which was shared by
Lagrange [1] and Euler, neither finding a solution, while the latter
asserted the existence of a resisting medium in space.

Again, in 1774, the Academy submitted the same subject, a third time,
for the prize; and again Lagrange failed to detect a cause in
gravitation.

Laplace [2] now took the matter in hand. He tried the effect of a
non-instantaneous action of gravity, to no purpose. But in 1787 he
gave the true explanation. The principal effect of the sun on the
moon's orbit is to diminish the earth's influence, thus lengthening
the period to a new value generally taken as constant. But Laplace's
calculations showed the new value to depend upon the excentricity of
the earth's orbit, which, according; to theory, has a periodical
variation of enormous period, and has been continually diminishing for
thousands of years. Thus the solar influence has been diminishing, and
the moon's mean motion increased. Laplace computed the amount at 10"
in one century, agreeing with observation. (Later on Adams showed that
Laplace's calculation was wrong, and that the value he found was too
large; so, part of the acceleration is now attributed by some
astronomers to a lengthening of the day by tidal friction.)

Another contribution by Halley to the verification of Newton's law was
made when he went to St. Helena to catalogue the southern stars. He
measured the change in length of the second's pendulum in different
latitudes due to the changes in gravity foretold by Newton.

Furthermore, he discovered the long inequality of Jupiter and Saturn,
whose period is 929 years. For an investigation of this also the
Academy of Sciences offered their prize. This led Euler to write a
valuable essay disclosing a new method of computing perturbations,
called the instantaneous ellipse with variable elements. The method
was much developed by Lagrange.

But again it was Laplace who solved the problem of the inequalities of

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