He stars and He-accreting CO white dwarfs

Details He stars and He-accreting CO white dwarfs He stars and He-accreting CO white dwarfs

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...371..317l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 371, April 10, 1991, p. 317-331.

Statistics

Computation

44

B Stars, Binary Stars, Carbon, Oxygen, Stellar Mass Accretion, White Dwarf Stars, Stellar Evolution, Stellar Models, Stellar Structure, Supernovae

Scientific paper

He star models in the mass range 0.4-1.0 solar mass have been evolved until the red giant phase or, depending on their mass, until crystallization on the white-dwarf cooling sequence. Some of the degenerate structures obtained in these computations have been successively accreted at various He accretion rates in order to better define the fate of the accreting dwarf versus its mass and accretion rate for a fixed degeneracy level of the accreting dwarf. He stars have been further induced to transfer mass to a degenerate companion through Roche lobe overflow, in conditions of large gravitational wave radiation by the system. CO dwarfs in binary systems with He stars are found to experience a thermal behavior whose effects are such to locate the structure on the verge of obtaining a strong SN-like explosive event.

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