Does magnetic field modify tidal dynamics in the convective envelope of Solar mass stars?
| Autor: | Astoul, Aur��lie, Mathis, St��phane, Baruteau, Cl��ment, Gallet, Florian, Augustson, Kyle C., Bolmont, Emeline, Brun, Allan S., Strugarek, Antoine |
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| Jazyk: | angličtina |
| Rok vydání: | 2018 |
| Předmět: |
Earth and Planetary Astrophysics (astro-ph.EP)
Astrophysics - Solar and Stellar Astrophysics FOS: Physical sciences Astrophysics::Solar and Stellar Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics::Earth and Planetary Astrophysics Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics::Galaxy Astrophysics Physics::Geophysics Astrophysics - Earth and Planetary Astrophysics |
| Popis: | The energy dissipation of wave-like tidal flows in the convective envelope of low-mass stars is one of the key physical mechanisms that shape the orbital and rotational dynamics of short-period planetary systems. Tidal flows, and the excitation, propagation, and dissipation of tidally-induced inertial waves can be modified by stellar magnetic fields (e.g., Wei 2016, 2018, Lin and Ogilvie 2018). It is thus important to assess for which stars, at which location of their internal structure, and at which phase of their evolution, one needs to take into account the effects of magnetic fields on tidal waves. Using scaling laws that provide the amplitude of dynamo-generated magnetic fields along the rotational evolution of these stars (e.g., Christensen et al. 2009, Brun et al. 2015), combined with detailed grids of stellar rotation models (e.g., Amard et al. 2016), we examine the influence of a magnetic field on tidal forcing and dissipation near the tachocline of solar-like stars. We show that full consideration of magnetic fields is required to compute tidal dissipation, but not necessarily for tidal forcing. 6 pages, 4 figures, SF2A 2018 proceeding |
| Databáze: | OpenAIRE |
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