Hostname: page-component-586b7cd67f-t7fkt Total loading time: 0 Render date: 2024-11-25T14:58:53.876Z Has data issue: false hasContentIssue false
  • English
  • Français

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

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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