Mass loss during nova outbursts for various white dwarf masses

Journal Article · Wed Nov 01 00:00:00 EST 1989 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/168022· OSTI ID:7265998

Kato, Mariko; Hachisu, Izumi ^[1]

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1. Keio Univ., Yokohama (Japan) Kyoto Univ. (Japan)

Six sequences of steady mass loss and static envelope models have been simulated for the white dwarf masses M(WD) = 0.4, 0.6, 0.7, 0.9, 1.0, and 1.2 solar mass. The hydrogen-rich envelope mass decreases from model to model as a result of wind mass loss and hydrogen burning. If solar chemical composition is assumed, it is found that optically thick wind occurs for M(WD) greater than 0.8 solar mass. Empirical formulae relating to mass-loss rate and the mass of the hydrogen-rich envelope are obtained for the sequences M(WD) = 0.9, 1.0, and 1.2 solar mass and used to estimate the evolutionary time scale of the decay phase, as well as the amount of the mass lost from the system. In order for a white dwarf to grow from 1.0 to 1.38 solar mass, the companion star should transfer more than 1.1 solar mass of matter to the white dwarf when the mass transfer rate is 1 x 10 to the -7th solar mass per yr, thus amounting to as much as 11 solar mass for 10 to the -10th solar mass per yr. 32 refs.

• OSTI ID: 7265998
• Journal Information: Astrophysical Journal; (USA), Vol. 346; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
NOVAE
WHITE DWARF STARS
MASS TRANSFER
BINARY STARS
CHEMICAL COMPOSITION
HYDROGEN BURNING
MASS
STAR EVOLUTION
STAR MODELS
STELLAR WINDS
SUPERNOVAE
DWARF STARS
ERUPTIVE VARIABLE STARS
MATHEMATICAL MODELS
STAR BURNING
STARS
STELLAR ACTIVITY
VARIABLE STARS
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources