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Colliding stellar winds: magnetic field structure in the interaction region

Published online by Cambridge University Press:  25 May 2016

Svetozar A. Zhekov ,
A.V. Myasnikov  and
E.V. Barsky
Svetozar A. Zhekov
Affiliation:
JILA, University of Colorado, Boulder, Colorado 80309-0440, USA
A.V. Myasnikov
Affiliation:
Institute for Problems in Mechanics, Russian Academy of Sciences 101 Vernadskii Ave., Moscow 117526, Russia
E.V. Barsky
Affiliation:
Institute for Problems in Mechanics, Russian Academy of Sciences 101 Vernadskii Ave., Moscow 117526, Russia

Abstract

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The geometry structure of the magnetic field in colliding stellar winds is studied. It is shown that the magnetic field influence in the interaction region depends mainly on the ratio of the wind ram pressures of the components, the ratio of the stellar linear rotational velocity to the wind velocity of the magnetized star, and the stellar separation. For the radiative colliding winds the magnetic field influence increases with the importance of the radiative losses. An asymmetric magnetic field structure appears for a given set of binary parameters and the interaction region might be an asymmetric source of non-thermal radio emission.

Type
Part 3. Interaction of Wolf-Rayet stars and other hot massive stars with their environment: colliding winds and ring nebulae
Information
Symposium - International Astronomical Union , Volume 193: Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies , 1999 , pp. 400 - 401
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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