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Dust Driven Winds from Pulsating Stars

Published online by Cambridge University Press:  12 April 2016

E.A. Dorfi ,
M.U. Feuchtinger  and
S. Höfner
E.A. Dorfi
Affiliation:
Institut für Astronomie der Universität Wien, Türkenschanzstr. 17, 1180 Wien, Austria
M.U. Feuchtinger
Affiliation:
Institut für Astronomie der Universität Wien, Türkenschanzstr. 17, 1180 Wien, Austria
S. Höfner
Affiliation:
Institut für Astronomie der Universität Wien, Türkenschanzstr. 17, 1180 Wien, Austria

Extract

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The cool extended atmospheres of late type giants are sites where dust formation takes place. Radiation pressure on the dust grains is an important force for driving the slow but massive winds observed in such objects. Existing calculations of dust driven stellar winds (e.g. Bowen 1988, Fleischer et al. 1991) suffer from the fact that they include approximations at various levels for different parts of the problem like the hydrodynamics or the dust formation. Furthermore they do not include time-dependent radiative transfer.

In order to overcome these insufficiencies we plan to calculate self-consistent models of dust driven winds with a full description of both the radiation hydrodynamics and the time-dependent dust formation. As a first step, however, we concentrate our investigations on the self-consistent description of the radiation hydrodynamics adopting only a simple description of the dust opacities.

Type
VI. Asteroseismology: theory
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 572 - 574
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

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