Stellar atmospheres : $b A contribution to the observational study of high temperature in the reversing layers of starsPayne-Gaposchkin, Cecilia
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Stellar atmospheres : $b A contribution to the observational study of high temperature in the reversing layers of stars
Payne-Gaposchkin, Cecilia
Astrophysics; Stars -- Spectra; Stars -- Temperature; Thesis (Ph. D.)
Two sets of sulphur lines, differing in astrophysical behavior, were
noted by Lockyer[272] at 4163, 4174, 4815, and at 4253, 4285, 4295.
These lines have been attributed by the writer,[273] and by Fowler and
Milne,[274] to S+ and S++ respectively. The S+ lines appear to be in
pairs, and the S++ lines suggest a triplet, although one of the three
lines is extremely faint in stellar spectra, and it would be expected
that the once and twice ionized spectra of sulphur would display even
and odd multiplicities respectively. The two series have maxima at
and at , but the stellar intensities of the lines are
small. An amplification of our knowledge of stellar sulphur is greatly
to be desired.
POTASSIUM (19)
The ultimate lines[275] of potassium () are at 7664
and 7699, and have been traced in the solar spectrum, although they
are very faint. They appear to be absent from the flash spectrum.[276]
Russell[277] expresses the opinion that they persist, with rising
temperature, as far as in the stellar sequence.
CALCIUM (20)
The element calcium is extensively represented in stellar spectra.
The ultimate line of the neutral atom is at 4227 () and
appears at . The line increases in strength in all cooler
stars, in accordance with theory, and has a distinct variation with
[Pg 71]
absolute magnitude. The , and
multiplets[278] are satisfactorily identified in the solar spectrum
and can be traced with certainty in the spectra of stars cooler than
. The , , , and lines
appear to be present with the appropriate intensities in the sun, but
are too faint to be seen with small dispersion. Thus all the classified
lines of calcium which are strong in laboratory spectra have been
traced in the spectra of the sun and stars.
IONIZED CALCIUM
The and lines of ionized calcium are seen throughout the
stellar sequence, and reach a maximum within the type,[279] where
their intensity is greater than that attained by any other line in any
class. They vary with absolute magnitude.[280] In the sun the lines
are doubly reversed, and they are probably singly reversed[281] in
61 Cygni.
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