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The Effects of Magnetic Fields on the Winds from Luminous Hot Stars

Published online by Cambridge University Press:  12 April 2016

Joseph P. Cassinelli  and
Nathan A. Miller
Joseph P. Cassinelli
Affiliation:
University of Wisconsin, Astronomy Department, 475 N. Charter St. Madison WI. 53706, USA
Nathan A. Miller
Affiliation:
University of Wisconsin, Astronomy Department, 475 N. Charter St. Madison WI. 53706, USA

Abstract

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Here we explore three types of models in which the combination of magnetic fields with line driving forces leads to faster winds than line forces alone. The fields can change the flow geometry; they can couple with rotation and transmit angular momentum; and they can carry transverse Alfvén waves. All three can lead to a deposition of momentum beyond the critical point and accelerate winds. Some history of the attempts to use magnetic fields to understand hot star winds is discussed and several new models for magnetic rotator B[e] winds are presented.

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. 169 - 177
Copyright
Copyright © Springer-Verlag 1999

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