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Towards a complete picture of the evolution of planetary systems around evolved stars

Published online by Cambridge University Press:  16 October 2024

Mats Esseldeurs Open the ORCID record for Mats Esseldeurs [Opens in a new window] ,
Stéphane Mathis  and
Leen Decin
Mats Esseldeurs*
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
Stéphane Mathis
Affiliation:
Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, 91191 Gif-sur-Yvette, France
Leen Decin
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
*
email: [email protected]
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Abstract

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Solar-like stars evolve through the Asymptotic Giant Branch (AGB) phase. This phase is characterized by increased radii, high luminosities, and significant mass loss. In order to understand the survival of companions during this phase, and explain the presence of planets orbiting white dwarfs, it is essential to examine the orbital evolution of these systems. Several physical mechanisms come into play for AGB stars, including stellar mass loss and tidal interactions between the star and its companion. Assessing mass-loss rates and accretion to the companion requires complex radiation-hydro-chemical simulations. Furthermore, comprehending the full history of tidal dissipation in low-mass stars during their late evolutionary stages, which strongly depends on their internal structure, requires dedicated analytical and numerical studies.

Keywords

AGB starsstellar winds and mass-losstidesstar-planet interactions
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S382: Complex Planetary Systems II: Latest Methods for an Interdisciplinary Approach , December 2022 , pp. 98 - 100
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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