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Fast Winds in Planetary Nebulae

Published online by Cambridge University Press:  18 September 2017

F. D. Kahn
F. D. Kahn*
Affiliation:
Department of Astronomy, The University, Manchester M13 9PL

Abstract

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A planetary nebula consists mainly of gas ejected slowly by a red giant. Its dynamics is dominated by the hot central star which is left behind later. In particular a fast wind from this star forms a bubble of hot gas which fills the inner part of the nebula and pushes the envelope into a shell. This shell remains only partly ionized for a considerable time. Its non-ionized part is subject to a Rayleigh-Taylor instability, and is expected to break up into fragments which remain behind in the HII part of the nebula.

Type
Section IV: Origin of Planetary Nebulae
Information
Symposium - International Astronomical Union , Volume 103: Planetary Nebulae , 1983 , pp. 305 - 316
Copyright
Copyright © Reidel 1983 

References

Cassinelli, J. P.: 1979, Ann. Rev. Astron. Astrophys., 17, 275.Google Scholar
Dyson, J. E.: 1978, Astron. Astrophys., 62, 269.Google Scholar
Habing, H. J.: 1983, contribution to this Symposium.Google Scholar
Kahn, F. D.: 1976, Astron. Astrophys., 50, 145.Google Scholar
Kwok, Sun: 1983, Paper given at this Symposium.Google Scholar
Lazareff, B.: 1981, “Role de la phase coronale dans la dynamique du milieu interstellaire”, , Universite Paris-Sud.Google Scholar