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Growth Rate of White Dwarf Mass in Binaries

Published online by Cambridge University Press:  12 April 2016

Mariko Kato ,
Hideyuki Saio  and
Izumi Hachisu
Mariko Kato
Affiliation:
Department of Astronomy, Keio University Kouhoku-ku, Yokohama 223Japan
Hideyuki Saio
Affiliation:
Department of Astronomy, University of Tokyo Bunkyou-ku, Tokyo 113Japan
Izumi Hachisu
Affiliation:
Department of Aeronautical Engineering, Kyoto University Sakyou-ku, Kyoto 606Japan

Abstract

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The growth rate of a white dwarf which accretes hydrogen-rich or helium matter is studied. If the accretion rate is relatively small, unstable shell flash occurs and during which the envelope mass is lost. We have followed the evolutions of shell flashes by steady state approach with wind mass loss solutions to determined the mass lost from the system for wide range of binary parameters. The time-dependent models are also calculated in some cases. The mass loss due to the Roche lobe overflow are taken into account. This results seriously affects the existing scenarios on the origin of the type I supernova or on the neutron star formation induced by accretion.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 114: White Dwarfs , 1989 , pp. 507 - 510
Copyright
Copyright © Springer-Verlag 1989

References

Kato, M. 1983, Pub. Astr. Soc. Japan, 35, 507.Google Scholar
Kato, M., and Hachisu, I. 1988a, Ap. J., 329, 808.Google Scholar
Kato, M., and Hachisu, I. 1988b, Ap . J., submitted.Google Scholar
Kato, M., Saio, H., and Haehisu, I. 1988, Ap. J., submitted.Google Scholar
Prialnik, D., 1986 Ap. J., 310, 222.Google Scholar
Taam, R.E., and van den Heuvel, E.P.J. 1986 Ap.J., 305, 235.CrossRefGoogle Scholar