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RGB mass loss: inferences from CMD-fitting and asteroseismology

Published online by Cambridge University Press:  30 November 2022

Marco Tailo Open the ORCID record for Marco Tailo [Opens in a new window]
Marco Tailo*
Affiliation:
Dipartimento di Fisica e Astronomia Augusto Righi, Università degli Studi di Bologna, Via Gobetti 93/2, I-40129 Bologna, Italy email: [email protected], [email protected]
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Abstract

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The amount of mass lost by stars during the red-giant branch (RGB) phase is one of the main parameters needed to fully understand later stages of stellar evolution. In spite of its importance, a fully-comprehensive physical understanding of this phenomenon is still missing, and we, mostly, rely on empirical formulations. The Galactic Globular Clusters are ideal targets to derive such formulations, but, until recently, the presence of multiple populations has been a major challenge.

We will discuss the insights on RGB mass loss that can be obtained from the study of the horizontal branch stars in such stellar associations. The estimates obtained via the study of the photometric data will be compared with recent and newly obtained estimates derived for few high metallicity open clusters and a large sample of field stars with asteroseismic techniques.

Keywords

stars: Hertzsprung-Russell diagramstars: horizontal-branchstars: mass lossstars: fundamental parameters
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S366: The Origin of Outflows in Evolved Stars , November 2020 , pp. 321 - 326
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Copyright
© The Author(s), 2022. Published by Cambridge University Press on behalf of International Astronomical Union

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