The thermal stability of hot degenerate stars in steady-state accretion

Details The thermal stability of hot degenerate stars in steady-state accretion The thermal stability of hot degenerate stars in steady-state accretion

Mar 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...220..636s&link_type=abstract

Astrophysical Journal, Part 1, vol. 220, Mar. 1, 1978, p. 636-639.

Astronomy and Astrophysics

Astrophysics

6

Hot Stars, Stellar Mass Accretion, Stellar Models, Thermal Stability, Stellar Envelopes, Stellar Evolution, Stellar Luminosity, Stellar Mass, Stellar Structure, Thermonuclear Reactions, Variable Stars, White Dwarf Stars, X Ray Sources

Scientific paper

Models of high-luminosity degenerate stars have been constructed in the mass range from 1.2 to 1.38 solar masses. They derive all of their energy from hydrogen burning near the surface in a steady state with accretion. The models have carbon-oxygen cores and envelopes composed of a hydrogen-helium mixture and a carbon-nitrogen abundance of 1% by mass. The thermal stability of these models is analyzed using both a linear analysis and evolutionary calculations. The models are thermally stable in all cases, with the stability increasing with increasing luminosity. The bearing of these results on X-ray sources and pulsations of white dwarfs driven by hydrogen shell burning is briefly discussed.

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