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The dissipation of the kinetic energy of wave-like tidal flows within theconvective envelope of low-mass stars is one of the key physical mechanismsthat shapes the orbital and rotational dynamics of short-period exoplanetarysystems. Although low-mass stars are magnetically active objects, the questionof how the star's magnetic field impacts large-scale tidal flows and theexcitation, propagation and dissipation of tidal waves still remains open. Ourgoal is to investigate the impact of stellar magnetism on the forcing of tidalwaves, and their propagation and dissipation in the convective envelope oflow-mass stars as they evolve. We have estimated the amplitude of the magneticcontribution to the forcing and dissipation of tidally induced magneto-inertialwaves throughout the structural and rotational evolution of low-mass stars(from M to F-type). For this purpose, we have used detailed grids of rotatingstellar models computed with the stellar evolution code STAREVOL. The amplitudeof dynamo-generated magnetic fields is estimated via physical scaling laws atthe base and the top of the convective envelope. We find that the large-scalemagnetic field of the star has little influence on the excitation of tidalwaves in the case of nearly-circular orbits and coplanar hot-Jupiter planetarysystems, but that it has a major impact on the way waves are dissipated. Ourresults therefore indicate that a full magneto-hydrodynamical treatment of thepropagation and dissipation of tidal waves is needed to properly assess theimpact of star-planet tidal interactions throughout the evolutionary history oflow-mass stars hosting short-period massive planets.

Does magnetic field impact tidal dynamics inside the convective zone of low-mass stars along their evolution?