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Dynamical Galactic Halos

Effect of Magnetic Field and Galactic Rotation

Published online by Cambridge University Press:  19 July 2016

D. Breitschwerdt ,
H.J. Völk ,
V. Ptuskin  and
V. Zirakashvili
D. Breitschwerdt
Affiliation:
Max-Planck-Institut für Kernphysik, Postfach 10 39 80, W-6900 Heidelberg, Germany
H.J. Völk
Affiliation:
Max-Planck-Institut für Kernphysik, Postfach 10 39 80, W-6900 Heidelberg, Germany
V. Ptuskin
Affiliation:
IZMIR AN, USSR Academy of Sciences, Troitsk, Moscow Region 142092, CIS
V. Zirakashvili
Affiliation:
IZMIR AN, USSR Academy of Sciences, Troitsk, Moscow Region 142092, CIS

Abstract

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It is argued that the description of the magnetic field in halos of galaxies should take into account its dynamical coupling to the other major components of the interstellar medium, namely thermal plasma and cosmic rays (CR's). It is then inevitable to have some loss of gas and CR's (galactic wind) provided that there exist some “open” magnetic field lines, facilitating their escape, and a sufficient level of self-generated waves which couple the particles to the gas. We discuss qualitatively the topology of the magnetic field in the halo and show how galactic rotation and magnetic forces can be included in such an outflow picture.

Keywords

Galactic HalosMagnetic FieldsCosmic Rays
Type
9. Magnetohydrodynamic Phenomena in the Interstellar Medium Related to Dynamo Processes
Information
Symposium - International Astronomical Union , Volume 157: The Cosmic Dynamo , 1993 , pp. 415 - 419
Copyright
Copyright © Kluwer 1993 

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