Mass-radius relations for white dwarf stars of different internal compositions

Details Mass-radius relations for white dwarf stars of different internal compositions Mass-radius relations for white dwarf stars of different internal compositions

1999-09-29

arxiv.org/abs/astro-ph/9909499v1

Astronomy and Astrophysics

Astrophysics

8 pages, 9 figures. Accepted for publication in Astronomy and Astrophysics

Scientific paper

The purpose of this work is to present accurate and detailed mass-radius relations for white dwarf (WD) models with helium, carbon, oxygen, silicon and iron cores, by using a fully updated stellar evolutionary code. We considered masses from 0.15 to 0.5 Mo for the case of helium core, from 0.45 to 1.2 Mo for carbon, oxygen and silicon cores and from 0.45 to 1.0 Mo for the case of an iron core. In view of recent measurements made by Hipparcos that strongly suggest the existence of WDs with an iron-dominated core, we focus our attention mainly on the finite-temperature, mass-radius relations for WD models with iron interiors. Furthermore, we explore the effects of gravitational, chemical and thermal diffusion on low-mass helium WD models with hydrogen and helium envelopes.

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