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Is the wind of the Oe star HD 155806 magnetically confined?

Published online by Cambridge University Press:  01 November 2008

Véronique Petit ,
A. W. Fullerton ,
S. Bagnulo  and
G. A. Wade
Véronique Petit
Affiliation:
Département de Physique, Université Laval, Québec, Canada
A. W. Fullerton
Affiliation:
Space Telescope Science Institute, Baltimore, USA
S. Bagnulo
Affiliation:
Armagh Observatory, Armagh, Northern Ireland
G. A. Wade
Affiliation:
Department Physics, Royal Military College of Canada, Kingston, Canada
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Abstract

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Oe stars are a subset of the O-type stars that exhibit emission lines from a circumstellar disk. The recent detection of magnetic fields in some O-type stars suggests a possible explanation for the stability of disk-like structures around Oe stars. According to this hypothesis, the wind of the star is channeled by a dipolar magnetic field producing a disc in the magnetic equatorial plane. As a test of this model, we have obtained spectropolarimetric observations of the hottest Galactic Oe star HD 155806. Here we discuss its results and implications.

Keywords

Stars: magnetic fields – stars: mass loss – stars: early-type – stars: emission-line

References

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