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Nova Explosion of Mass Accreting White Dwarfs

Published online by Cambridge University Press:  12 April 2016

Ken’ichi Nomoto ,
Kyoji Nariai  and
Daiichiro Sugimoto
Ken’ichi Nomoto
Affiliation:
Department of Physics, Ibaraki University
Kyoji Nariai
Affiliation:
Tokyo Astronomical Observatory, University of Tokyo
Daiichiro Sugimoto
Affiliation:
Department of Earth Science and Astronomy, College of General Education, University of Tokyo

Extract

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Evolution of a mass accreting white dwarf has been computed from the onset of accretion through nova explosion. We have considered a white dwarf of 1.3M⊙ with the accretion rate of 1×10-10M⊙ yr-1. Because the thermal structure during the accretion phase has been fully taken into computation, the mass of the accreted hydrogen-rich envelope and the corresponding temperature distribution in the envelope have been determined. When the hydrogen-rich envelope of mass ΔMH = 1.63 × 10-4M⊙ has been formed, a hydrogen-shell flashes commences. The flashing shell lies midway between the bottom of the envelope and the stellar surface; the mass lying above this shell is 5.7 × 10-5M⊙

Type
Abstracts of Workshop Papers on Novae
Information
International Astronomical Union Colloquium , Volume 53: White Dwarfs and Variable Degenerate Stars , August 1979 , pp. 529
Copyright
Copyright © The University of Rochester 1979