Reference : New advances in asteroseismology of pulsating hot subdwarf stars
Scientific congresses and symposiums : Paper published in a journal
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
New advances in asteroseismology of pulsating hot subdwarf stars
Charpinet, S. mailto [Laboratoire d'Astrophysique de Toulouse-Tarbes, Université de Toulouse, CNRS, 14 av. E. Belin, 31400 Toulouse, France]
Van Grootel, Valérie mailto [Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Astrophysique stellaire théorique et astérosismologie]
Randall, S. K. [ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany]
Green, E. M. [Steward Observatory, University of Arizona, 933 North Cherry Ave., Tucson, AZ 85721]
Fontaine, G. [Université de Montréal, C.P. 6128, Succ. Centre-Ville, Montréal, QC H3C 3J7, Canada]
Brassard, P. [Université de Montréal, C.P. 6128, Succ. Centre-Ville, Montréal, QC H3C 3J7, Canada]
Chayer, P. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA]
Highlights of Astronomy
International Astronomical Union
International Astronomical Union
[en] stars:subdwarfs ; stars:oscillations ; stars:interiors ; stars:rotation
[en] Hot subdwarf stars (of the sdB and sdO type) host three known classes of nonradial pulsators. Two of them feature short period (P ~ 60 - 600 s) accoustic mode oscillations, while the third group is characterized by slow g-mode deformations with periods of ~ 1 - 2h. These pulsations offer favorable grounds to infer some of the internal properties of these objects through asteroseismology. This has been exploited for the rapid p-mode sdB pulsators and the present contribution reviews some of the recent advances in this field. The long period g-mode pulsators, whose vibrations probe much deeper inside the star, are also of high interest. With the advent of space observations using CoRoT and KEPLER, the asteroseismology of these slower oscillators will also become a possibility, and likely contribute to significant breakthroughs in our understanding of these hot and compact stars.

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