Great Astronomers by Robert Stawell Ball (best ereader for students .txt) 📖
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falls upon it. Notwithstanding that a star is a sun thousands of
times larger than the planet and millions of times more remote,
yet it is a singular fact that telescopic planets possess an
illusory resemblance to the stars among which their course happens
to lie. So far as actual appearance goes, there is indeed only
one criterion by which a planet of this kind can be discriminated
from a star. If the planet be large enough the telescope will
show that it possesses a disc, and has a visible and measurable
circular outline. This feature a star does not exhibit. The
stars are indeed so remote that no matter how large they may be
intrinsically, they only exhibit radiant points of light, which
the utmost powers of the telescope fail to magnify into objects
with an appreciable diameter. The older and well-known planets,
such as Jupiter and Mars, possess discs, which, though not visible
to the unaided eye, were clearly enough discernible with the
slightest telescopic power. But a very remote planet like Uranus,
though it possessed a disc large enough to be quickly appreciated
by the consummate observing skill of Herschel, was nevertheless so
stellar in its appearance, that it had been observed no fewer than
seventeen times by experienced astronomers prior to Herschel. In
each case the planetary nature of the object had been overlooked,
and it had been taken for granted that it was a star. It
presented no difference which was sufficient to arrest attention.
As the unknown body by which Uranus was disturbed was certainly
much more remote than Uranus, it seemed to be certain that though
it might show a disc perceptible to very close inspection, yet
that the disc must be so minute as not to be detected except with
extreme care. In other words, it seemed probable that the body
which was to be sought for could not readily be discriminated from
a small star, to which class of object it bore a superficial
resemblance, though, as a matter of fact, there was the
profoundest difference between the two bodies.
There are on the heavens many hundreds of thousands of stars, and
the problem of identifying the planet, if indeed it should lie
among these stars, seemed a very complex matter. Of course it is
the abundant presence of the stars which causes the difficulty.
If the stars could have been got rid of, a sweep over the heavens
would at once disclose all the planets which are bright enough to
be visible with the telescopic power employed. It is the
fortuitous resemblance of the planet to the stars which enables it
to escape detection. To discriminate the planet among stars
everywhere in the sky would be almost impossible. If, however,
some method could be devised for localizing that precise region in
which the planet’s existence might be presumed, then the search
could be undertaken with some prospect of success.
To a certain extent the problem of localizing the region on the
sky in which the planet might be expected admitted of an immediate
limitation. It is known that all the planets, or perhaps I ought
rather to say, all the great planets, confine their movements to a
certain zone around the heavens. This zone extends some way on
either side of that line called the ecliptic in which the earth
pursues its journey around the sun. It was therefore to be
inferred that the new planet need not be sought for outside this
zone. It is obvious that this consideration at once reduces the
area to be scrutinized to a small fraction of the entire heavens.
But even within the zone thus defined there are many thousands of
stars. It would seem a hopeless task to detect the new planet
unless some further limitation to its position could be assigned.
It was accordingly suggested to Le Verrier that he should
endeavour to discover in what particular part of the strip of the
celestial sphere which we have indicated the search for the
unknown planet should be instituted. The materials available to
the mathematician for the solution of this problem were to be
derived solely from the discrepancies between the calculated
places in which Uranus should be found, taking into account the
known causes of disturbance, and the actual places in which
observation had shown the planet to exist. Here was indeed an
unprecedented problem, and one of extraordinary difficulty. Le
Verrier, however, faced it, and, to the astonishment of the world,
succeeded in carrying it through to a brilliant solution.
We cannot here attempt to enter into any account of the
mathematical investigations that were necessary. All that we can
do is to give a general indication of the method which had to be
adopted.
Let us suppose that a planet is revolving outside Uranus, at a
distance which is suggested by the several distances at which the
other planets are dispersed around the sun. Let us assume that
this outer planet has started on its course, in a prescribed path,
and that it has a certain mass. It will, of course, disturb the
motion of Uranus, and in consequence of that disturbance Uranus
will follow a path the nature of which can be determined by
calculation. It will, however, generally be found that the path
so ascertained does not tally with the actual path which
observations have indicated for Uranus. This demonstrates that
the assumed circumstances of the unknown planet must be in some
respects erroneous, and the astronomer commences afresh with an
amended orbit. At last after many trials, Le Verrier ascertained
that, by assuming a certain size, shape, and position for the
unknown Planet’s orbit, and a certain value for the mass of
the hypothetical body, it would be possible to account for the
observed disturbances of Uranus. Gradually it became clear to
the perception of this consummate mathematician, not only that
the difficulties in the movements of Uranus could be thus
explained, but that no other explanation need be sought for. It
accordingly appeared that a planet possessing the mass which
he had assigned, and moving in the orbit which his calculations
had indicated, must indeed exist, though no eye had ever beheld
any such body. Here was, indeed, an astonishing result. The
mathematician sitting at his desk, by studying the observations
which had been supplied to him of one planet, is able to
discover the existence of another planet, and even to assign the
very position which it must occupy, ere ever the telescope is
invoked for its discovery.
Thus it was that the calculations of Le Verrier narrowed greatly
the area to be scrutinised in the telescopic search
which was presently to be instituted. It was already known, as we
have just pointed out, that the planet must lie somewhere on
the ecliptic. The French mathematician had now further
indicated the spot on the ecliptic at which, according to his
calculations, the planet must actually be found. And now for an
episode in this history which will be celebrated so long as
science shall endure. It is nothing less than the telescopic
confirmation of the existence of this new planet, which had
previously been indicated only by mathematical calculation. Le
Verrier had not himself the instruments necessary for studying the
heavens, nor did he possess the skill of the practical astronomer.
He, therefore, wrote to Dr. Galle, of the Observatory at Berlin,
requesting him to undertake a telescopic search for the new planet
in the vicinity which the mathematical calculation had indicated
for the whereabouts of the planet at that particular time. Le
Verrier added that he thought the planet ought to admit of being
recognised by the possession of a disc sufficiently definite to
mark the distinction between it and the surrounding stars.
It was the 23rd September, 1846, when the request from Le Verrier
reached the Berlin Observatory, and the night was clear, so that
the memorable search was made on the same evening. The
investigation was facilitated by the circumstance that a diligent
observer had recently compiled elaborate star maps for certain
tracts of the heavens lying in a sufficiently wide zone on both
sides of the equator. These maps were as yet only partially
complete, but it happened that Hora. XXI., which included the very
spot which Le Verrier’s results referred to, had been just issued.
Dr. Galle had thus before his, eyes a chart of all the stars which
were visible in that part of the heavens at the time when the map
was made. The advantage of such an assistance to the search could
hardly be overestimated. It at once gave the astronomer another
method of recognising the planet besides that afforded by its
possible possession of a disc. For as the planet was a moving
body, it would not have been in the same place relatively to the
stars at the time when the map was constructed, as it occupied
some years later when the search was being made. If the body
should be situated in the spot which Le Verrier’s calculations
indicated in the autumn of 1846, then it might be regarded
as certain that it would not be found in that same place on a
map drawn some years previously.
The search to be undertaken consisted in a comparison made point
by point between the bodies shown on the map, and those stars in
the sky which Dr. Galle’s telescope revealed. In the course of
this comparison it presently appeared that a star-like object of
the eighth magnitude, which was quite a conspicuous body in the
telescope, was not represented in the map. This at once attracted
the earnest attention of the astronomer, and raised his hopes that
here was indeed the planet. Nor were these hopes destined to be
disappointed. It could not be supposed that a star of the eighth
magnitude would have been overlooked in the preparation of a chart
whereon stars of many lower degrees of brightness were set down.
One other supposition was of course conceivable. It might have
been that this suspicious object belonged to the class of
variables, for there are many such stars whose brightness
fluctuates, and if it had happened that the map was constructed at
a time when the star in question had but feeble brilliance, it
might have escaped notice. It is also well known that sometimes
new stars suddenly develop, so that the possibility that what
Dr. Galle saw should have been a variable star or should have been
a totally new star had to be provided against.
Fortunately a test was immediately available to decide whether
the new object was indeed the long sought for planet, or whether
it was a star of one of the two classes to which I have just
referred. A star remains fixed, but a planet is in motion.
No doubt when a planet lies at the distance at which this new
planet was believed to be situated, its apparent motion would be
so slow that it would not be easy to detect any change in the
course of a single night’s observation. Dr. Galle, however,
addressed himself with much skill to the examination of the place
of the new body. Even in the course of the night he thought he
detected slight movements, and he awaited with much anxiety the
renewal of his observations on the subsequent evenings. His
suspicions as to the movement of the body were then amply
confirmed, and the planetary nature of the new object was thus
unmistakably detected.
Great indeed was the admiration of the scientific world
at this superb triumph. Here was a mighty planet whose very
existence was revealed by the indications afforded by refined
mathematical calculation. At once the name of Le Verrier, already
known to those conversant with the more profound branches of
astronomy, became everywhere celebrated. It soon, however,
appeared, that the
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