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Core Overshoot and Nonrigid Internal Rotation of Massive Stars: Current Status from Asteroseismology†

Published online by Cambridge University Press:  01 December 2007

Conny Aerts
Conny Aerts*
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium IMAPP, Radboud Universiteit Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, the Netherlands email: conny@ster.kuleuven.be
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Abstract

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Seismic estimates of core overshoot have been derived from extensive high-precision photometric and spectroscopic ground-based (multisite) campaigns for five main-sequence B-type stars. For three of these, the ratio of the near-core rotation frequency to the surface rotation frequency could be estimated as well, from the identified oscillation modes. We summarise these seismic results obtained for B stars. Now that the technique of asteroseismology was proven to work for probing the interior of massive stars, we expect a drastic increase in the precision of the structure parameters from the space missions CoRoT and Kepler, as well as from currently ongoing ground-based campaigns, in the coming years.

Keywords

stars: early-type – stars: oscillations – stars: evolution – stars: interiors – convection – line: profiles – techniques: spectroscopic – techniques: photometric – methods: data analysis – stars: fundamental parameters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S250: Massive Stars as Cosmic Engines , December 2007 , pp. 237 - 244
Copyright
Copyright © International Astronomical Union 2008

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