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New magnetic field measurements of β Cephei stars and slowly pulsating B stars

Published online by Cambridge University Press:  01 November 2008

Swetlana Hubrig ,
M. Briquet ,
P. De Cat ,
M. Schöller ,
T. Morel  and
I. Ilyin
Swetlana Hubrig
Affiliation:
ESO, Santiago, Chile; email: shubrig@eso.org
M. Briquet
Affiliation:
Katholieke Universiteit Leuven, Belgium
P. De Cat
Affiliation:
Koninklijke Sterrenwacht van België, Brussel, Belgium
M. Schöller
Affiliation:
ESO, Garching, Germany
T. Morel
Affiliation:
Université de Liège, Belgium
I. Ilyin
Affiliation:
Astrophysikalisches Institut Potsdam, Potsdam, Germany
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Abstract

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We present the results of the continuation of our magnetic survey with FORS 1 at the VLT of a sample of B-type stars consisting of confirmed or candidate β Cephei stars and Slowly Pulsating B stars. Roughly one third of the studied β Cephei stars have detected magnetic fields. The fraction of magnetic Slowly Pulsating B and candidate Slowly Pulsating B stars is found to be higher, up to 50%. We find that the domains of magnetic and non-magnetic pulsating stars in the H-R diagram largely overlap, and no clear picture emerges as to the possible evolution of the magnetic field across the main sequence.

Keywords

Stars: variables: β Cephei – stars: variables: SPBs – stars: oscillations – stars: Hertzsprung-Russell diagram, stars: magnetic fields, techniques: polarimetric – stars: ξ1 CMa

References

Hubrig, S., Briquet, M., Schöller, M., et al. 2006, MNRAS 369, L61CrossRefGoogle Scholar