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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 θ1 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.

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