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Modelling the Mass Loss of Cool AGB Stars

Published online by Cambridge University Press:  26 May 2016

Peter Woitke
Peter Woitke*
Affiliation:
Zentrum für Astronomie und Astrophysik, Technische Universität Berlin, Hardenbergstraße 36, Sekr. PN 8-1, D-10623 Berlin

Abstract

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The current status of modelling the wind driving mechanism of AGB stars is reviewed. Our present understanding of these winds is substantially guided by spherically symmetric, time-dependent models which reveal a complex interplay between stellar pulsation, hydrodynamics, small-scale waves, chemistry, dust formation and radiative transfer. The level of approximation used for the physical description of the various processes, and the degree of consistence in the models are crucial and different approaches lead to rather different results. Beside reviewing the frontiers of the present theoretical research on AGB star winds, this paper presents some new results concerning the cooling of the gas behind propagating shock waves in the outer atmosphere and the self-organisation of dust-forming gases (cloud formation) caused by a radiative/thermal instability of dust forming gases.

Type
Session F. Winds - Cool and Pulsating Stars
Information
Symposium - International Astronomical Union , Volume 210: Modelling of Stellar Atmospheres , 2003 , pp. 387 - 401
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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