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The Cyclic Evolution of Classical Novae

Published online by Cambridge University Press:  12 April 2016

Dina Prialnik
Dina Prialnik*
Affiliation:
Department of Geophysics and Planetary Sciences, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Ramat Aviv 69978, Israel

Extract

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The cyclic evolution of classical novae (CN) cannot be observed, as in the case of recurrent or dwarf novae. The duration of a typical cycle may range from a few thousand to a few 105 years. Thus we have to rely on theoretical studies for understanding the periodic outbursts — due to thermonuclear runaways (TNR) — on the surface of accreting white dwarfs (WD). One may distinguish between two kinds of studies: a) detailed investigations of a specific aspect or a particular evolutionary phase; b) studies which emphasize the cyclic behavior of novae and their long-term evolution. The latter, which form the subject of this brief review, may be divided into four groups, each adopting a different approach to the problem:

  1. 1. Steady-state (semi-analytic) solutions;

  2. 2. One- (or two-) zone models;

  3. 3. Quasi-static (and/or steady burning) numerical calculations;

  4. 4. Full-scale hydrodynamic evolutionary computations.

Type
3. Theory
Information
International Astronomical Union Colloquium , Volume 122: Physics of Classical Novae , 1990 , pp. 351 - 360
Copyright
Copyright © Springer-Verlag 1990

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