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

Published online by Cambridge University Press:  12 July 2011

Alex W. Fullerton ,
Véronique Petit ,
Stefano Bagnulo  and
Gregg A. Wade
Alex W. Fullerton
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA email: [email protected]
Véronique Petit
Affiliation:
Dept. of Geology & Astronomy, West Chester University, West Chester, PA 19383, USA email: [email protected]
Stefano Bagnulo
Affiliation:
Armagh Observatory, College Hill, Armagh, BT61 9DG, Northern Ireland email: [email protected]
Gregg A. Wade
Affiliation:
Dept. of Physics, Royal Military College of Canada, Kingston, ON, K7K 4B4, Canada email: [email protected]
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Abstract

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Spectropolarimetric observations of HD 155806 – the hottest Galactic Oe star – were obtained with CFHT/ESPaDOnS to test the hypothesis that disk signatures in its spectrum are due to magnetic channeling and confinement of its stellar wind. We did not detect a dipole field of sufficient strength to confine the wind, and could not confirm previous reports of a magnetic detection. It appears that stellar magnetism is not responsible for producing the disk of HD 155806.

Keywords

stars: early-typestars: emission-lineBestars: windsoutflowsstars: magnetic fieldsstars: individual (HD 155806)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 182 - 183
Copyright
Copyright © International Astronomical Union 2011

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