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Origin and pulsation of hot subdwarfs

Published online by Cambridge University Press:  18 February 2014

S. K. Randall ,
G. Fontaine ,
S. Charpinet ,
V. Van Grootel  and
P. Brassard
S. K. Randall
Affiliation:
ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany email: srandall@eso.org
G. Fontaine
Affiliation:
Département de Physique, Université de Montréal, C.P. 6128, Succ. Centre-Ville, Montréal, QC H3C 3J7, Canada
S. Charpinet
Affiliation:
CNRS, Université de Toulouse, UPS-OMP, IRAP, 14 av. E. Belin, 31400, Toulouse, France
V. Van Grootel
Affiliation:
Institut d'Astrophysique et de Géophysique de l'Université de Liège, Allée du 6 Août 17, B-4000 Liège, Belgium
P. Brassard
Affiliation:
Département de Physique, Université de Montréal, C.P. 6128, Succ. Centre-Ville, Montréal, QC H3C 3J7, Canada
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Abstract

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We briefly introduce hot subdwarfs and their evolutionary status before discussing the different types of known pulsators in more detail. Currently, at least six apparently distinct types of variable are known among hot subdwarfs, encompassing p- as well as g-mode pulsators and objects in the Galactic field as well as in globular clusters. Most of the oscillations detected can be explained in terms of an iron opacity mechanism, and quantitative asteroseismology has been very successful for some of the pulsators. In addition to helping constrain possible evolutionary scenarios, studies focussing on stellar pulsations have also been used to infer planets and characterize the rotation of the host star.

Keywords

stars: oscillationssubdwarfs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 289 - 296
Copyright
Copyright © International Astronomical Union 2014 

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