2018/11/21 by Aurélie Astoul, S. Mathis, Astoul, Aurélie +15
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Astro and Planetary Science #Earth and Planetary Astrophysics (astro-ph.EP) #FOS: Physical sciences #Geomagnetism and Paleomagnetism Studies #Solar and Space Plasma Dynamics #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies
paper · pdf · doi:10.48550/arxiv.1811.08649
openalex publication_date 2018/11/21 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The energy dissipation of wave-like tidal flows in the convective envelope of\nlow-mass stars is one of the key physical mechanisms that shape the orbital and\nrotational dynamics of short-period planetary systems. Tidal flows, and the\nexcitation, propagation, and dissipation of tidally-induced inertial waves can\nbe modified by stellar magnetic fields (e.g., Wei 2016, 2018, Lin and Ogilvie\n2018). It is thus important to assess for which stars, at which location of\ntheir internal structure, and at which phase of their evolution, one needs to\ntake into account the effects of magnetic fields on tidal waves. Using scaling\nlaws that provide the amplitude of dynamo-generated magnetic fields along the\nrotational evolution of these stars (e.g., Christensen et al. 2009, Brun et al.\n2015), combined with detailed grids of stellar rotation models (e.g., Amard et\nal. 2016), we examine the influence of a magnetic field on tidal forcing and\ndissipation near the tachocline of solar-like stars. We show that full\nconsideration of magnetic fields is required to compute tidal dissipation, but\nnot necessarily for tidal forcing.\n