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Mass Loss in Evolved Stars

Published online by Cambridge University Press:  07 February 2024

Lynn D. Matthews Open the ORCID record for Lynn D. Matthews [Opens in a new window]
Lynn D. Matthews*
Affiliation:
Massachusetts Institute of Technology Haystack Observatory, 99 Millstone Road, Westford, MA 01886 USA.
*
email: lmatthew@mit.edu
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Abstract

Intense mass loss through cool, low-velocity winds is a defining characteristic of low-to-intermediate mass stars during the asymptotic giant branch (AGB) evolutionary stage. Such winds return up ∼80% of the initial stellar mass to the interstellar medium and play a major role in enriching it with dust and heavy elements. A challenge to understanding the physics underlying AGB mass loss is its dependence on an interplay between complex and highly dynamic processes, including pulsations, convective flows, shocks, magnetic fields, and opacity changes resulting from dust and molecule formation. I highlight some examples of recent advances in our understanding of late-stage stellar mass loss that are emerging from radio and (sub)millimeter observations, with a particular focus on those that resolve the surfaces and extended atmospheres of evolved stars in space, time, and frequency.

Keywords

stars: AGBstars: mass lossstars: windsoutflowsmasers
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S380: Cosmic Masers: Proper Motion toward the Next-Generation Large Projects , December 2022 , pp. 275 - 291
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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