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Magnetic fields and pulsation in B and Be stars

Published online by Cambridge University Press:  17 November 2003

J. Arnaud ,
N. Meunier ,
C. Neiner ,
H. F. Henrichs ,
A.-M. Hubert ,
M. Floquet  and
V. C. Geers
C. Neiner
Affiliation:
Sterrenkundig Instituut Anton Pannekoek, Universiteit van Amsterdam, Kruislaan 403, 1998 SJ Amsterdam, The Netherlands Observatoire de Meudon, France
H. F. Henrichs
Affiliation:
Sterrenkundig Instituut Anton Pannekoek, Universiteit van Amsterdam, Kruislaan 403, 1998 SJ Amsterdam, The Netherlands
A.-M. Hubert
Affiliation:
Observatoire de Meudon, France
M. Floquet
Affiliation:
Observatoire de Meudon, France
V. C. Geers
Affiliation:
Sterrenkundig Instituut Anton Pannekoek, Universiteit van Amsterdam, Kruislaan 403, 1998 SJ Amsterdam, The Netherlands
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Abstract

We have searched for magnetic fields in several early B-type stars: βCephei, Slowly Pulsating B (SPB) and in particular Be stars. We recall the properties of these stars and highlight the problem of the Be phenomenon. We discuss two clues towards understanding this phenomenon in terms of pulsations and magnetic fields. We summarize results from spectropolarimetric observations obtained at the Pic du Midi (France) and highlight the results for the Be star ω Ori and the β Cep star V2052 Oph.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 9: Magnetism and Activity of the Sun and Stars , 2003 , pp. 257
Copyright
© EAS, EDP Sciences, 2003

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