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Galactic Winds

Published online by Cambridge University Press:  12 April 2016

Heinrich J. Völk ,
D. Breitschwerdt  and
J. F. McKenzie
Heinrich J. Völk
Affiliation:
Max-Planck-Institut für Kernphysik, Heidelberg
D. Breitschwerdt
Affiliation:
Max-Planck-Institut für Kernphysik, Heidelberg
J. F. McKenzie
Affiliation:
Max-Planck-Institut für Aeronomie, Lindau

Extract

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In the sequel we will be discussing that - apart from all other halo flows - it is highly probable that our Galaxy has a systematic mass loss; most other galaxies should behave in a similar way. This mass loss should occur in the form of a supersonic galactic wind provided the intergalactic pressure is low enough. We will investigate this possibility mainly for our Galaxy. We shall argue [1] that the energetic particle component of the interstellar medium, the cosmic rays (CRs), is basically responsible for driving a wind for typical gas temperatures below 106 K. Thus for asymptotic wind velocities of the order of the escape velocity, the mass flux is essentially determined by the observable CR energy loss from the Galaxy. Galaxies with very hot gas on the other hand hardly need the CR component and drive a wind almost exclusively through their thermal pressure.

Type
VI. Interstellar Matter at High Galactic Latitudes
Information
International Astronomical Union Colloquium , Volume 120: Structure and Dynamics of the Interstellar Medium , 1989 , pp. 448 - 453
Copyright
Copyright © Springer-Verlag 1989

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