The story of the universe. Volume 1 (of 4) : $b The starry skies
History
The story of the universe. Volume 1 (of 4) : $b The starry skies
Astronomy; Earth (Planet); Natural history
The sun outweighs fully seven hundred and forty times the combined
mass of all the planets which circle around him, so that, when we
regard the energy of his attraction, we still find him a worthy ruler
of the planetary scheme.
Viewed with the naked eye, the sun appears only as a luminous mass of
intense and uniform brightness; but when examined with the telescope,
his surface is frequently observed to be mottled over with a number
of dark spots, of irregular and ill-defined forms, constantly
varying in appearance, situation, and magnitude. These spots are
occasionally of immense size, so as to be visible even without the
aid of the telescope; and their number is frequently so great that
they occupy a considerable portion of the sun’s surface. Sir W.
Herschel observed one in 1779 the diameter of which exceeded 50,000
miles, more than six times the diameter of the earth; and Scheiner
affirms that he has seen no less than fifty on the sun’s disk at
once. Most of them have a deep black nucleus, surrounded by a fainter
shade, or _umbra_, of which the inner part, nearest to the nucleus,
is brighter than the exterior portion. The boundary between the
nucleus and umbra is in general tolerably well defined; and beyond
the umbra a stripe of light appears more vivid than the rest of the
sun.
[Illustration: Fig. 30.—Phase of Spot]
The discovery of the sun’s spots has been attributed to Fabricius,
Galileo, and Scheiner, and has been claimed for the English
astronomer Harriot. Amid these conflicting pretensions it is perhaps
impossible to arrive at the truth; but the matter is of little
importance; the discovery is one which followed inevitably that of
the telescope, and an accidental priority of observation can hardly
be considered as establishing any claim to merit.
The study of solar physics may be said to have commenced with the
discovery of the sun spots, about two hundred and sixty years ago.
These spots were presently found to traverse the solar disk in such
a way as to indicate that the sun turns upon an axis once in about
twenty-six days. Nor will this rotation appear slow, when we remember
that it implies a motion of the equatorial parts of the sun’s surface
at a rate exceeding some seventy times the motion of our swiftest
express train.
Next came the discovery that the solar spots are not surface stains,
but deep cavities in the solar substance. The changes of appearance
presented by the spots as they traverse the solar disk led Dr. Wilson
to form this theory so far back as 1779; but, strangely enough, it
is only in comparatively recent times that the hypothesis has been
finally established, since even within the last ten years a theory
was put forward which accounted satisfactorily for most of the
changes of appearance observed in the spots, by supposing them to be
due to solar clouds hanging suspended at a considerable elevation
above the true photosphere.
Public-domain text, read in full here on John Shaqi.
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