2016/11/24 by Émeline Bolmont, Emeline Bolmont, F. Gallet +11
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Dissipation #Earth and Planetary Astrophysics (astro-ph.EP) #FOS: Physical sciences #Geomagnetism and Paleomagnetism Studies #Geometry #Inertial wave #Metallicity #Physics #Planet #Planetary system #Rotation (mathematics) #Solar and Stellar Astrophysics (astro-ph.SR) #Stars #Stellar rotation #Stellar, planetary, and galactic studies #Tidal acceleration #Wave propagation #astro-ph.EP #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.1611.08243
published in arXiv (Cornell University) (Cornell University) · Submitted proceeding for the Astrofluid conference in honor of Jean-Paul Zahn (Paris, June 2016). 10 pages, 3 figures
arxiv created 2016/11/24 · openalex publication_date 2016/11/24 · arxiv updated 2016/11/28 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
Since 1995, numerous close-in planets have been discovered around low-mass\nstars (M to A-type stars). These systems are susceptible to be tidally\nevolving, in particular the dissipation of the kinetic energy of tidal flows in\nthe host star may modify its rotational evolution and also shape the orbital\narchitecture of the surrounding planetary system. Recent theoretical studies\nhave shown that the amplitude of the stellar dissipation can vary over several\norders of magnitude as the star evolves, and that it also depends on the\nstellar mass and rotation. We present here one of the first studies of the\ndynamics of close-in planets orbiting low-mass stars (from 0.6~M_ odot to\n1.2~M_ odot) where we compute the simultaneous evolution of the star's\nstructure, rotation and tidal dissipation in its external convective envelope.\nWe demonstrate that tidal friction due to the stellar dynamical tide, i.e.\ntidal inertial waves (their restoring force is the Coriolis acceleration)\nexcited in the convection zone, can be larger by several orders of magnitude\nthan the one of the equilibrium tide currently used in celestial mechanics.\nThis is particularly true during the Pre Main Sequence (PMS) phase and to a\nlesser extent during the Sub Giant (SG) phase. Numerical simulations show that\nonly the high dissipation occurring during the PMS phase has a visible effect\non the semi-major axis of close-in planets. We also investigate the effect of\nthe metallicity of the star on the tidal evolution of planets. We find that the\nhigher the metallicity of the star, the higher the dissipation and the larger\nthe tidally-induced migration of the planet.\n