Steady state models of white dwarfs accreting helium or carbon/oxygen-rich matter

Details Steady state models of white dwarfs accreting helium or carbon/oxygen-rich matter Steady state models of white dwarfs accreting helium or carbon/oxygen-rich matter

May 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...328..207k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 328, May 1, 1988, p. 207-212.

Astronomy and Astrophysics

Astrophysics

19

Nuclear Reactions, Steady State, Stellar Interiors, Stellar Mass Accretion, Stellar Models, White Dwarf Stars, Binary Stars, Gas Mixtures, Giant Stars, Stellar Cores, Stellar Evolution

Scientific paper

The authors have calculated steady state models of white dwarfs which accrete helium or carbon/oxygen (C+O)-rich matter. The helium accreting model consists of a highly degenerate C+O core and a helium burning shell, overlaid by a helium envelope. The C+O accreting model consists of a highly degenerate O+Ne+Mg core, a carbon burning shell, and a C+O envelope. For the C+O accreting white dwarfs, there exist minimum accretion rates below which no steady state solution exists. For accretion rates above the minimum value, there exist two branches of solutions: compact and normal branches. All the models in the compact branch are thermally unstable.

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