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Discovery of Non-Radial Pulsations in the White Dwarf Primary of a Cataclysmic Variable Star

Published online by Cambridge University Press:  08 February 2017

Brian Warner  and
Liza Van Zyl
Brian Warner
Affiliation:
Department of Astronomy, University of Cape Town, Rondebosch 7700. South Africa
Liza Van Zyl
Affiliation:
Department of Astronomy, University of Cape Town, Rondebosch 7700. South Africa

Extract

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Non-radial pulsations in isolated white dwarfs have been known for 25 years and it has been shown that the hydrogen-rich (DA) white dwarfs have a high probability of pulsating if they lie in the instability strip with effective temperature between 11500 and 13200 K - the ZZ Ceti stars (e.g. Kepler and Nelan 1993). Analysing techniques developed for such stars allow derivation of masses, luminosities, rotation periods, hydrogen surface layer masses and other properties (e.g. Kepler and Bradley 1995). A number of binary systems are known in which the primary is a white dwarf; dominant in this class are the cataclysmic variable (CV) stars. Until now no CV primary has been found to have non-radial pulsations.

Type
V. Asteroseismology I
Information
Symposium - International Astronomical Union , Volume 185: New Eyes to See Inside the Sun and Stars , 1998 , pp. 321 - 322
Copyright
Copyright © Kluwer 1998 

References

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