Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...291..812k&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 291, April 15, 1985, p. 812-821.
Astronomy and Astrophysics
Astrophysics
65
Abundance, Stellar Composition, Stellar Mass Accretion, White Dwarf Stars, Carbon, Ejecta, Heavy Elements, Nitrogen, Oxygen, Stellar Cores, Stellar Models, Thermonuclear Reactions
Scientific paper
The configurations of potential nova progenitors at the onset of a thermonuclear runaway (TNR) are obtained by evolving a series of white dwarf (WD) models through the quasi-static accretion phase preceding the TNR. Special attention is paid to the effect of diffusion on composition profiles. The initial parameters of the accretion phase are the WD mass, the WD luminosity, and the accretion rate. They lead to a wide range of combinations of accreted mass and heavy element content of the envelope Z(env). It is found that the WD mass is the most important parameter in determining the accreted mass. A lower limit exists for the mass of a WD capable of producing a nova-like outburst which decreases with decreasing WD mass. There is a strong correlation between the accretion rate and Z(env), higher Z(env) values resulting from lower accretion rates. Changes in WD luminosity have no dramatic effect on the outcome of the accretion phase.
Kovetz Attay
Prialnik Dina
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