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Can the stellar dynamical tide destabilize the resonant chains of planets formed in the disk?

Published online by Cambridge University Press:  16 October 2024

Leon Ka Wang Kwok Open the ORCID record for Leon Ka Wang Kwok [Opens in a new window] ,
Emeline Bolmont ,
Alexandre Revol ,
Stéphane Mathis ,
Aurélie Astoul ,
Corinne Charbonnel  and
Sean Raymond
Leon Ka Wang Kwok*
Affiliation:
Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland
Emeline Bolmont
Affiliation:
Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland
Alexandre Revol
Affiliation:
Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland
Stéphane Mathis
Affiliation:
Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, 91191, Gif-sur-Yvette, France
Aurélie Astoul
Affiliation:
Department of Applied Mathematics, School of Mathematics, University of Leeds, Leeds LS2 9JT, UK
Corinne Charbonnel
Affiliation:
Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland
Sean Raymond
Affiliation:
Laboratoire d’Astrophysique de Bordeaux, CNRS and Université de Bordeaux, Allée Geoffroy St. Hilaire, 33165 Pessac, France
*
email: leon.kawang.kwok@gmail.com
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Abstract

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Evolution models of planetary systems find that resonant chains of planets often arise from the formation within protoplanetary disks. However, the occurrence of observed resonant chains, such as the notable TRAPPIST-1 system, is relatively low. This suggests that the majority of these chains become destabilized after the dissipation of the protoplanetary disk. Stellar tides, especially the wavelike dynamical tide, could be proposed as potential contributors to the destabilization of resonant chains. The dissipation of the dynamical tide, because of the frequency-dependant tidal excitation of stellar oscillation eigenmodes, potentially leads to a boost in migration for the close-in planets and disrupts the fragile stability of resonant chains. Thus, we investigate the influence of the stellar dynamical tide on multi-planet systems with taking their dissipation into account in the N-body code Posidonius. Notably, this research represents the first exploration of the impact of frequency-dependent dynamical tides on multi-planet systems.

Keywords

star-planet interactionsplanetary dynamicsmean motion resonances (MMRs)resonant chainstidal interactionsstellar tidesdynamical tides
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. 146 - 148
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Creative Commons
Creative Common License - CCCreative Common License - BYCreative Common License - NCCreative Common License - ND
This is an Open Access article, distributed under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives licence (http://creativecommons.org/licenses/by-nc-nd/4.0/), which permits non-commercial re-use, distribution, and reproduction in any medium, provided that no alterations are made and the original article is properly cited. The written permission of Cambridge University Press must be obtained prior to any commercial use and/or adaptation of the article.
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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