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

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arxiv 0812.2464 v1 pith:GAEQ3NBB submitted 2008-12-12 astro-ph

V. Petit , A. W. Fullerton , S. Bagnulo , G. A. Wade (for the MiMeS Collaboration) This is my paper
classification astro-ph
keywords starsmagneticstaro-typeobservationswindaccordingaround
verification ladder T0 review T1 audit T2 compute T3 formal
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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 the results and implications of those observations.

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