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Title:
Model atmospheres of red degenerate stars
Authors:
Kapranidis, S.
Affiliation:
AA(Washington, University, Seattle, WA; Iowa State University of Science and Technology, Ames, IA)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 275, Dec. 1, 1983, p. 342-353. (ApJ Homepage)
Publication Date:
12/1983
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Stellar Atmospheres, Stellar Models, Stellar Temperature, White Dwarf Stars, Atmospheric Density, Chemical Composition, Equations Of State, Helium, Optical Thickness, Temperature Dependence, Thomas-Fermi Model
DOI:
10.1086/161537
Bibliographic Code:
1983ApJ...275..342K

Abstract

Cool white dwarf star model atmospheres in the T(eff) range of 2500-6000 K are calculated, under the assumption of a pure helium chemical composition and a g value of 100 million cm/sec-squared. In the photospheres of white dwarfs cooler than 4000 K, pressure ionization and electron degeneracy become increasingly important as T(eff) decreases. Electron thermal conduction also becomes important for these temperatures, yielding a large temperature gradient reduction in the layers above the convection zone and a reduction of the height of the top of the convection zone so that, as T(eff) decreases, the upper boundary of the convection zone sinks deeper into the atmosphere. It is also found that the density of the atmospheres of these very cool white dwarfs is large, even at very low optical depths, implying an atmospheric structure with a massive but transparent layer close to the surface which adds little to optical depth.

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