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The Effect of a Close Binary Companion on a Nova Outburst
Published online by Cambridge University Press: 12 April 2016
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We compare two hydrodynamic calculations of thermonuclear runaways in material accreted by a 1M⊙ white dwarf of initial luminosity 10−3L⊙. In both cases the CNO abundances are taken to be near solar (ZCNO = 0.014). The only difference between the calculations is that in one sequence of models (seq.B) the additional energy generation due to the interaction between the expanding nova envelope and a close red dwarf companion is allowed for, using a simple model based on that of Paczynski (1976).
- Type
- Abstracts of Workshop Papers on Novae
- Information
- International Astronomical Union Colloquium , Volume 53: White Dwarfs and Variable Degenerate Stars , August 1979 , pp. 531
- Copyright
- Copyright © The University of Rochester 1979
References
Paczynski, B.
1976, in I.A.U. Symposium No. 73, p. 751, ed. by Eggleton, , Mitton, and Whelan, .Google Scholar
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