Evolution of white dwarfs

Details Evolution of white dwarfs Evolution of white dwarfs

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...154..125k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 154, no. 1-2, Jan. 1986, p. 125-134.

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135

Stellar Evolution, White Dwarf Stars, Computational Astrophysics, Equations Of State, Stellar Luminosity, Stellar Mass, Stellar Structure

Scientific paper

The evolution of white dwarfs with 0.598 and 0.546 M_sun; is followed from the stage of a central star of planetary nebulae to very low luminosities using a stellar evolution code, realistic initial models and equation of state. Since the authors' model end up with a somewhat smaller hydrogen envelope mass than found in a recent paper by Iben and Tutukov (1984) they do not find a late phase where hydrogen burning is the dominant energy source. The reason for this difference and implications concerning the amount of hydrogen present in cool white dwarfs are discussed. The main emphasis is, however, on the deviations of radii and surface gravities from the Hamada and Salpeter (1961) zero temperature models. These deviations are large at effective temperatures above 40000K and have to be taken into account in the determination of masses and space densities for white dwarfs.

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