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Asteroseismic observations of OB stars

Published online by Cambridge University Press:  12 July 2011

Peter De Cat ,
Katrien Uytterhoeven ,
Juan Gutiérrez-Soto ,
Pieter Degroote  and
Sergio Simón-Díaz
Peter De Cat
Affiliation:
Royal observatory of Belgium, Ringlaan 3, B-1180 Brussel, Belgium email: [email protected]
Katrien Uytterhoeven
Affiliation:
Lab. AIM, CEA/DSM-CNRS-Université Paris Diderot, CEA, IRFU, SAp, Saclay, 91191, Gif-sur-Yvette, France email: [email protected]
Juan Gutiérrez-Soto
Affiliation:
Instituto de Astrofísica de Andalucía (CSIC), Apartado 3004, 18080 Granada, Spain email: [email protected]
Pieter Degroote
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium email: [email protected]
Sergio Simón-Díaz
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain email: [email protected]
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Abstract

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The region of the hot end of the main-sequence is hosting pulsating stars of different types and flavours. Pulsations are not only observed for Slowly pulsating B stars (mid to late B-type stars; high order g-modes) and β Cephei stars (early B-type stars; low order p/g-modes) but are also causing variability in Be stars and OB-supergiants. In this review we give an overview of the asteroseismic observations that are currently available for these types of stars. The first asteroseismic results were solely based on ground-based observations. Recently, the arrival of space-based data gathered by space missions like most, corot and kepler has led to important discoveries for massive stars, highlighting their excellent asteroseismic potential. We show that, despite the unprecedented precision of the space-based data, there is still a clear need for ground-based follow-up observations.

Keywords

stars: early-typestars: emission-lineBestars: variables: otherstars: oscillations (including pulsations)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 433 - 444
Copyright
Copyright © International Astronomical Union 2011

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