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Paris Diderot - IRFU/DAp, Centre de Saclay, 91191, Gif-sur-Yvette Cedex, France" } ], "person_or_org": { "family_name": "Brun", "given_name": "Sacha A.", "name": "Brun, Sacha A.", "type": "personal" } }, { "affiliations": [ { "name": "Observatoire de Gen\u00e8ve, Universit\u00e9 de Gen\u00e8ve, 51 Chemin des Maillettes, CH-1290 Sauverny, Switzerland" } ], "person_or_org": { "family_name": "Bolmont", "given_name": "Emeline", "name": "Bolmont, Emeline", "type": "personal" } } ], "description": "
Over 4000 exoplanets have been discovered in the past 25 years or so, most of which orbit cool stars. Star-planet tidal interactions are known to drive the late evolution of the shortest-period planetary systems via tidal dissipation. Such dissipation is known to vary considerably with the mass, age, rotation, and metallicity of the star. To quantify tidal dissipation as accurately as possible, two key physical mechanisms need to be further explored : stellar differential rotation and magnetism in convective regions, which have been constrained in cool stars by ground-based spectropolarimetric observations as well as space-based asteroseismic observations.
\nIn this contribution, we report our recent progress on the investigation of the impact of stellar differential rotation and magnetism on the dynamics and dissipation of tidal inertial waves, along the evolution of low-mass stars. First, we show that a large-scale magnetic field has a negligible effect on the excitation of tidal waves whereas it deeply impacts the dissipation mechanism of tidal waves in the convective envelope of all cool stars all along their evolution. Then, by developing a local shearing box model of a small patch of the convective shell, we demonstrate how tidal waves can be either fully transmitted, damped, or even amplified at the so-called critical layers (when the phase speed of the wave is equal to the local velocity of the fluid), that has potentially strong implications for angular momentum exchanges between tidal waves and zonal flows, and ultimately for the evolution of planetary systems.
Contributions are accepted from participants that presented invited plenary session reviews, contributed plenary session talks, short "Haiku" talks and contributed posters. In addition, individual and collective contributions from (parallel) Topical Interest Rooms are welcome. If you would like to submit a typical conference proceeding, there are no formal page limits. For guidance we recommend you limit yourself to 4-8 pages for contributed talks and 10-15 pages for invited talks. Those wishing to submit a written conference proceeding are encouraged to format the document using the CS20 LaTeX template (available on https://github.com/CoolStars20/proceedings/releases/latest). All such submissions should be made as PDFs and will be reviewed for content by the SOC and we may suggest edits.
\r\n\r\nSubmission of presentation slides from speakers and full posters are also encouraged. PDF versions of these documents are the preferred format for Zenodo contributions to permit the documents to be previewed in a web browser. For maximum impact, a written contribution may be provided with presentation slides and/or a poster to provide greater context. Contributions will be checked for the proper metadata. Instructions about how to prepare your contribution are available on http://coolstars20.cfa.harvard.edu/contributions.html
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