A Popular History of Astronomy During the Nineteenth Century: Fourth EditionClerke, Agnes M. (Agnes Mary)
History
A Popular History of Astronomy During the Nineteenth Century: Fourth Edition
Clerke, Agnes M. (Agnes Mary)
Astronomy -- History -- 19th century
This first attempt to assign the part played in cosmical physics by
chemical affinities was marked by the importation into the theory of the
sun of the now familiar phrase _dissociation_. It is indeed tolerably
certain that no such combinations as those contemplated by Faye occur at
the photospheric level, since the temperature there must be enormously
higher than would be needed to reduce all metallic earths and oxides;
but molecular changes of some kind, dependent perhaps in part upon
electrical conditions, in part upon the effects of radiation into space,
most likely replace them. The conjecture was emitted by Dr. Johnstone
Stoney in 1867[441] that the photospheric clouds are composed of
carbon-particles precipitated from their mounting vapour just where the
temperature is lowered by expansion and radiation to the boiling-point
of that substance. But this view, though countenanced by Ångström,[442]
and advocated by Hastings of Baltimore,[443] and other authorities,[444]
is open to grave objections.[445]
In Faye's theory, sun-spots were regarded as simply breaks in the
photospheric clouds, where the rising currents had strength to tear them
asunder. It followed that they were regions of increased heat--regions,
in fact, where the temperature was too high to permit the occurrence of
the precipitations to which the photosphere is due. Their obscurity was
attributed, as in Dr. Brester's more recent _Théorie du Soleil_, to
deficiency of emissive power. Yet here the verdict of the spectroscope
is adverse and irreversible.
After every deduction, however, has been made, we still find that
several ideas of permanent value were embodied in this comprehensive
sketch of the solar constitution. The principal of these were; first,
that the sun is a mainly gaseous body; secondly, that its stores of heat
are rendered available at the surface by means of vertical
convection-currents--by the bodily transport, that is to say, of
intensely hot matter upward, and of comparatively cool matter downward;
thirdly, that the photosphere is a surface of condensation, forming the
limit set by the cold of space to this circulating process, and that a
similar formation must attend, at a certain stage, the cooling of every
cosmical body.
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