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The most massive pulsating white dwarf stars

Published online by Cambridge University Press:  18 February 2014

Barbara G. Castanheira  and
S. O. Kepler
Barbara G. Castanheira
Affiliation:
Department of Astronomy and McDonald Observatory, University of Texas Austin, TX 78712, USA email: barbara@astro.as.utexas.edu
S. O. Kepler
Affiliation:
Instituto de Física, Universidade Federal do Rio Grande do Sul 91501-970 Porto Alegre, RS, Brazil email: kepler@if.ufrgs.br
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Abstract

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Massive pulsating white dwarf stars are extremely rare, because of their small size and because they are the final product of high-mass stars, which are less common. Because of their intrinsic smaller size, they are fainter than the normal size white dwarf stars. The motivation to look for this type of stars is to be able to study in detail their internal structure and also derive generic properties for the sub-class of variables, the massive ZZ Ceti stars. Our goal is to investigate whether the internal structures of these stars differ from the lower-mass ones, which in turn could have been resultant from the previous evolutionary stages.

In this paper, we present the ensemble seismological analysis of the known massive pulsating white dwarf stars. Some of these pulsating stars might have substantial crystallized cores, which would allow us to probe solid physics in extreme conditions.

Keywords

stars: oscillations (including pulsations)stars: white dwarfs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 281 - 284
Copyright
Copyright © International Astronomical Union 2014 

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