EDP Sciences
Free access
Issue
A&A
Volume 398, Number 1, January IV 2003
Page(s) 253 - 266
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20021643


A&A 398, 253-266 (2003)
DOI: 10.1051/0004-6361:20021643

Three-component modeling of C-rich AGB star winds

I. Method and first results
C. Sandin and S. Höfner

Department of Astronomy and Space Physics, Uppsala University, Box 515, 751 20 Uppsala, Sweden
(Received 28 May 2002 / Accepted 7 November 2002 )

Abstract
Radiative acceleration of newly-formed dust grains and transfer of momentum from the dust to the gas plays an important role for driving winds of AGB stars. Therefore a detailed description of the interaction of gas and dust is a prerequisite for realistic models of such winds. In this paper we present the method and first results of a three-component time-dependent model of dust-driven AGB star winds. With the model we plan to study the role and effects of the gas-dust interaction on the mass loss and wind formation. The wind model includes separate conservation laws for each of the three components of gas, dust and the radiation field and is developed from an existing model which assumes position coupling between the gas and the dust. As a new feature we introduce a separate equation of motion for the dust component in order to fully separate the dust phase from the gas phase. The transfer of mass, energy and momentum between the phases is treated by interaction terms. We also carry out a detailed study of the physical form and influence of the momentum transfer term (the drag force) and three approximations to it. In the present study we are interested mainly in the effect of the new treatment of the dust velocity on dust-induced instabilities in the wind. As we want to study the consequences of the additional freedom of the dust velocity on the model we calculate winds both with and without the separate dust equation of motion. The wind models are calculated for several sets of stellar parameters. We find that there is a higher threshold in the carbon/oxygen abundance ratio at which winds form in the new model. The winds of the new models, which include drift, differ from the previously stationary winds, and the winds with the lowest mass loss rates no longer form.


Key words: hydrodynamics -- radiative transfer -- instabilities -- stars: AGB and post-AGB -- stars: mass-loss

Offprint request: C. Sandin, Christer.Sandin@astro.uu.se




© ESO 2003