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Making a Be star: the role of rotation and pulsations

Published online by Cambridge University Press:  18 February 2014

Coralie Neiner  and
Stéphane Mathis
Coralie Neiner
Affiliation:
LESIA, UMR 8109 du CNRS, Observatoire de Paris, UPMC, Univ. Paris Diderot 5 place Jules Janssen, 92195 Meudon Cedex, France email: coralie.neiner@obspm.fr
Stéphane Mathis
Affiliation:
LESIA, UMR 8109 du CNRS, Observatoire de Paris, UPMC, Univ. Paris Diderot 5 place Jules Janssen, 92195 Meudon Cedex, France email: coralie.neiner@obspm.fr Laboratoire AIM Paris-Saclay, CEA/DSM-CNRS-Université Paris Diderot IRFU/SAp, Centre de Saclay, 91191 Gif-sur-Yvette Cedex, France email: stephane.mathis@cea.fr
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Abstract

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The Be phenomenon, i.e. the ejection of matter from Be stars into a circumstellar disk, has been a long lasting mystery. In the last few years, the CoRoT satellite brought clear evidence that Be outbursts are directly correlated to pulsations and rapid rotation. In particular the stochastic excitation of gravito-inertial modes, such as those detected by CoRoT in the hot Be star HD 51452, is enhanced thanks to rapid rotation. These waves increase the transport of angular momentum and help to bring the already rapid stellar rotation to its critical value at the surface, allowing the star to eject material. Below we summarize the recent observational and theoretical findings and describe the new picture of the Be phenomenon which arose from these results.

Keywords

stars: emission-lineBestars: mass lossstars: oscillations (including pulsations)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 465 - 466
Copyright
Copyright © International Astronomical Union 2014 

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