New model atmospheres for very cool white dwarfs with mixed H/He and pure He compositions

Details New model atmospheres for very cool white dwarfs with mixed H/He and pure He compositions New model atmospheres for very cool white dwarfs with mixed H/He and pure He compositions

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...443..764b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 443, no. 2, p. 764-779

Astronomy and Astrophysics

Astrophysics

148

Abundance, Atmospheric Models, Helium, Hydrogen, Ionization, Pressure Effects, Stellar Atmospheres, White Dwarf Stars, Absorption Cross Sections, Atomic Collisions, Chemical Composition, Equations Of State, Molecular Collisions, Stellar Color, Stellar Gravitation, Stellar Temperature

Scientific paper

New model atmosphere calculations for very cool white dwarfs with mixed H/He and pure He compositions are presented. The hydrogen-rich models incorporate improved cross section calculations of the collision-induced absorption by molecular hydrogen due to collisions with H2, H, and He. The effects associated with variations in the effective temperature (Teff greater than or equal to 4000 and less than or equal to 10,000 K), the surface gravity (log g greater than or equal to 7.5 and less than or equal to 9.5), and the chemical composition (N(He)/N(H) greater than or equal to O and less than or equal to 100) are investigated. Results from earlier calculations are confirmed qualitatively, but a more detailed comparison reveals large quantitative deviations. Cool white dwarfs with mixed H/He chemical compositions are shown to be easily recognizable from their predicted strong infrared flux deficiency. Pure helium model calculations are described as well. These include a modified version of the recently developed equation of state of D. Saumon and G. Chabrier. Nonideal effects brought about by various equations of state are explored in detail. For the purpose of this analysis, a model of pressure ionization based on an accurate description of the interactions in a mostly atomic helium fluid is developed. The effects of pressure ionization are shown to be the most important issue in the model calculations. A critical discussion of previous generations of pure helium model calculations is presented. Finally, broadband color indices are provided for the complete model grid.

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