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Atmospheric structure and dynamics of evolved massive stars. Thanks to 3D radiative hydrodynamical simulations of stellar convection

Published online by Cambridge University Press:  30 November 2022

A. Chiavassa Open the ORCID record for A. Chiavassa [Opens in a new window]
A. Chiavassa*
Affiliation:
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Lagrange, CS 34229, Nice, France email: andrea.chiavassa@oca.eu Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, 85741 Garching, Germany
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Abstract

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Evolved massive stars are major cosmic engines, providing strong mechanical and radiative feedback on their host environment. They contribute to the enrichment of their environment through a strong stellar winds, still poorly understood. Wind physics across the life cycle of these stars is the key ingredient to accomplish a complete understanding of their evolution in the near and distant Universe. Nowadays, the development of the observational instruments is so advanced that the observations became very sensitive to the details of the stellar surface making possible to quantitatively study what happens on their surfaces and above where the stellar winds become dominant. Three-dimensional radiative hydrodynamics simulations of evolved stars are essential to a proper and quantitative analysis of these observations. This work presents how these simulations have been (and will be) crucial to prepare and interpret a multitude of observations and how they are important to achieve the knowledge of the mass-loss mechanism.

Keywords

Massive evolved starshydrodynamicsradiative transfer
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S366: The Origin of Outflows in Evolved Stars , November 2020 , pp. 101 - 116
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Copyright
© The Author(s), 2022. Published by Cambridge University Press on behalf of International Astronomical Union

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