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X-Ray Emission from Magnetically Confined Winds

Published online by Cambridge University Press:  12 April 2016

Jacques Babel
Jacques Babel*
Affiliation:
Battieux 36, 2000 Neuchatel, Switzerland

Abstract

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We consider the effect of large scale magnetic fields on the circumstellar environment of hot stars. In these stars, magnetic fields of order of 100 G lead to magnetically confined wind shocks (MCWS) and then to the existence of large X-ray emitting region. MCWS lead also to the presence of corotating cooling disks around hot stars.

We discuss the case of θ 1 Ori C, which is perhaps the hottest analog to Bp stars and consider the effect from rotation and instabilities. We finally discuss the case of the Herbig Ae-Be HD 104237 and show that MCWS might also explain the X-ray emission from this star.

Information

Type
Section II Theory of Non-spherical Winds
Information
International Astronomical Union Colloquium , Volume 169: Variable and Non-spherical Stellar Winds in Luminous Hot Stars , 1999 , pp. 187 - 190
Copyright
Copyright © Springer-Verlag 1999

References

Babel, J., Montmerle, T. (1997a), A&A 323, 121 Google Scholar
Babel, J., Montmerle, T. (1997b), Apj 485, L29 Google Scholar
Donati, J.-F., Wade, G.A.:(1998), A&A in pressGoogle Scholar
Donati, J.-F.:1998, Thèse d’habilitation, Univ. Toulouse III Google Scholar
Gagné, M., et al. (1997), Apj 478, L87 Google Scholar
Stahl, O., et al. (1996), A&A 312, 539 Google Scholar