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Explaining the winds of AGB stars: Recent progress

Published online by Cambridge University Press:  30 November 2022

Susanne Höfner Open the ORCID record for Susanne Höfner [Opens in a new window]  and
Bernd Freytag Open the ORCID record for Bernd Freytag [Opens in a new window]
Susanne Höfner
Affiliation:
Theoretical Astrophysics, Department of Physics & Astronomy, Uppsala University, Box 516, SE-75120 Uppsala, Sweden email: susanne.hoefner@physics.uu.se
Bernd Freytag
Affiliation:
Theoretical Astrophysics, Department of Physics & Astronomy, Uppsala University, Box 516, SE-75120 Uppsala, Sweden email: susanne.hoefner@physics.uu.se
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Abstract

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The winds observed around asymptotic giant branch (AGB) stars are generally attributed to radiation pressure on dust, which is formed in the extended dynamical atmospheres of these pulsating, strongly convective stars. Current radiation-hydrodynamical models can explain many of the observed features, and they are on the brink of delivering a predictive theory of mass loss. This review summarizes recent results and ongoing work on winds of AGB stars, discussing critical ingredients of the driving mechanism, and first results of global 3D RHD star-and-wind-in-a-box simulations. With such models it becomes possible to follow the flow of matter, in full 3D geometry, all the way from the turbulent, pulsating interior of an AGB star, through its atmosphere and dust formation zone into the region where the wind is accelerated by radiation pressure on dust. Advanced instruments, which can resolve the stellar atmospheres, where the winds originate, provide essential data for testing the models.

Keywords

stars: AGB and post-AGBstars: atmospheresstars: windsoutflowsstars: mass losscircumstellar matter
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S366: The Origin of Outflows in Evolved Stars , November 2020 , pp. 165 - 172
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Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2022. Published by Cambridge University Press on behalf of International Astronomical Union

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