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.)
ADDITIONAL DEDUCTIONS FROM
IONIZATION THEORY
[Pg 155]
CHAPTER XI
THE ASTROPHYSICAL EVALUATION OF PHYSICAL CONSTANTS
IN the opening chapter the statement was made that “the astrophysicist
is obliged to assume [the validity of physical laws] in applying them
to stellar conditions.” The astrophysical evaluation of physical
constants might therefore seem, from our avowed premises, to involve
a circular argument. In certain special cases, however, the process
appears to be legitimate, and the results of three investigations are
contained in the present chapter. The first of these investigations
involves the derivation of spectroscopic constants, assuming the series
formula; the second consists of an extrapolation of the results of
Chapter X to the estimation of unknown ionization potentials; and the
third constitutes a discussion made possible by the knowledge of the
stellar atmosphere that has been attained with the aid of ionization
theory.
THE RYDBERG CONSTANT FOR HELIUM
The wave-lengths of a series of lines can be measured in the spectrum
of a star, and the series identified with a series observed in the
laboratory. The occurrence in stellar spectra of series that can be
identified with the series given by terrestrial atoms presumably
shows that similar relations govern the atomic processes in the two
sources. That series formulae of the same type are applicable to the
stellar and terrestrial atom is indeed rather an observational fact
than an assumption. By inserting into the appropriate series formula
the observed stellar frequencies, a physical constant involved may be
evaluated, and the extent of the agreement with the corresponding value
from the laboratory may be determined.
[Pg 156]
H. H. Plaskett[429] has measured the wave-lengths of the lines of the
Pickering series () of He+ in the spectra of three
stars, incidentally separating the alternate Pickering lines from
the Balmer lines for the first time. The formula that connects the
frequencies of the lines with the constants associated with the atom is
Plaskett discussed the theory, and derived from the measured
wave-lengths of five lines the mean value of 109722.3 ± 0.44 for the
constant . The value determined in the laboratory by Paschen
is 109722.14 ± 0.04. Plaskett’s comment on the agreement is as
follows: “It was not to be expected that there would be any startling
changes.... It is of interest, however, to note that these “stellar”
determinations are in agreement with the terrestrial values, in
so far as it shows that the implicit assumption of identical atomic
structure, identical electrons, and identical laws of radiation on the
earth and in the stars, is in some measure justified.”
CRITICAL POTENTIALS
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