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Dust-driven Winds Beyond Spherical Symmetry

Published online by Cambridge University Press:  01 April 2008

Peter Woitke
Peter Woitke*
Affiliation:
UK Astronomy Technology Centre, Blackford Hill, EH9 3HJ Edinburgh, Scotland, UK School of Physics & Astronomy, University of St Andrews, North Haugh, KY16 9SS St. Andrews, Scotland, UK, email: ptw@roe.ac.uk
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Abstract

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New 2D dynamical models for the winds of AGB stars are presented which include hydrodynamics with radiation pressure on dust, equilibrium chemistry, time-dependent dust formation theory, and coupled frequency-dependent Monte Carlo radiative transfer. The simulations reveal a much more complicated picture of the dust formation and wind acceleration as compared to 1D spherical wind models. Triggered by non-spherical pulsations or large-scale convective motions, dust forms event-like in the cooler regions above the stellar surface which are temporarily less illuminated, followed by the radial ejection of dust arcs and clumps. These simulations can possibly explain recent high angular resolution interferometric IR observations of red giants, which show an often non-symmetric and highly time-variable innermost dust formation and wind acceleration zone. The dependence of the mass-loss rates on stellar parameters is less threshold-like as used from 1D models, and therefore, it seems quite possible that the phenomenon of dust-driven winds may occur also in less evolved red giants.

Keywords

hydrodynamicsradiative transferstars: late-typestars: windsstars: mass loss
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 229 - 234
Copyright
Copyright © International Astronomical Union 2008

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