Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...346..424k&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 346, Nov. 1, 1989, p. 424-434.
Astronomy and Astrophysics
Astrophysics
35
Novae, Stellar Mass Ejection, White Dwarf Stars, Binary Stars, Mass Flow Rate, Stellar Composition, Stellar Winds, Supernovae
Scientific paper
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.
Hachisu Izumi
Kato Mariko
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