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Turbulent Mixing in Circumstellar Space in the Presence of Magnetic Fields

Published online by Cambridge University Press:  19 July 2016

D. Breitschwerdt  and
F.D. Kahn
D. Breitschwerdt
Affiliation:
† Max-Planck-Institut für Kernphysik, D-6900 Heidelberg, FRG
F.D. Kahn
Affiliation:
‡ Department of Astronomy, Manchester MIS 9PL, England

Abstract

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The magnetic field structure in the swept-up HII shell and the stellar wind region around an early type star is described. It is argued that the field does not become dynamically so important as to prevent self-similar flow. A condition under which reconnexion removes magnetic energy from the bubble is derived. It follows that the process of turbulent mixing between the HII region and the bubble works efficiently enough to cause severe departures from uniform expansion, even in the presence of magnetic fields.

Type
4. Magnetohydrodynamics of Galactic Magnetic Fields
Information
Symposium - International Astronomical Union , Volume 140: Galactic and Intergalactic Magnetic Fields , 1990 , pp. 163 - 167
Copyright
Copyright © Kluwer 1990 

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