Mass-radius relations for low-mass white dwarfs with helium and carbon interiors.

Details Mass-radius relations for low-mass white dwarfs with helium and carbon interiors. Mass-radius relations for low-mass white dwarfs with helium and carbon interiors.

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...296..117v&link_type=abstract

Astronomy and Astrophysics, v.296, p.117

Astronomy and Astrophysics

Astrophysics

19

Stars: Binaries: Close, Stars: White Dwarfs, Stars: Interiors, Stars: Evolution, Stars: Feige 24

Scientific paper

We have computed static mass-radius relations for low-mass white dwarfs defined by surface gravities in the range g=10^7^-10^8^cm/s^2^. We have assumed pure helium interiors without a hydrogen envelope and carbon interiors with and without a hydrogen envelope. Surface boundary conditions also assume non-zero effective temperatures at 49,000<=T_eff_<=61,000K. Although generally applicable to isolated low-mass white dwarfs, these models are particularly interesting for the interpretation of the class of low-mass He white dwarfs that potentially emerge from close binary evolution. We discuss in particular the case of Feige 24 for which Vennes & Thorstensen (1994a) have proposed a low mass and large radius based on their gravitational redshift measurement. The binary parameters of Feige 24 are consistent with the population of He white dwarf + red dwarf close binaries predicted by theory but also with a population having a more common carbon interior with a thick hydrogen envelope. We demonstrate that a thin hydrogen layer is unlikely.

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