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Stability of Accreting White Dwarfs in Close Binary Systems

Published online by Cambridge University Press:  12 April 2016

R. Sienkiewicz  and
W. Dziembowski
R. Sienkiewicz
Affiliation:
N. Copernicus Astronomical Center, Polish Academy of Sciences, Aleje Ujazdowskie 4, 00-478 Warszawa, POLAND
W. Dziembowski
Affiliation:
N. Copernicus Astronomical Center, Polish Academy of Sciences, Aleje Ujazdowskie 4, 00-478 Warszawa, POLAND

Abstract

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We present results of thermal and vibrational stability analysis for 1 M⊙ white dwarf models corresponding to various accretion rates ≳ 10−11 M⊙/y. Accretion is assumed to be spherically symmetric and stationary. Thermal instability due to nuclear burning of hydrogen (at lower accretion rates) and helium (at higher rates) was found. At medium rates two growing thermal modes are simultaneously present. Vibrational instability was found for all models except those corresponding to highest accretion rates. The excitation rates for some nonradial g-modes are at least 3 orders of magnitude higher than those for radial pulsations. These rates are also higher than the excitation rates for thermal modes in certain range of accretion rates corresponding to high luminosities and effective temperatures. Among objects in which these instabilities may be important are symbiotic stars and nuclei of planetary nebulae.

Type
Part II: Cataclysmic Variables
Information
International Astronomical Union Colloquium , Volume 42: The Interaction of Variable Stars with their Environment , 1977 , pp. 327 - 339
Copyright
Copyright © Veröff. Der Remeis-Sterwarte 1977

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