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Star-planet interactions must be taken into account in stellar models tounderstand the dynamical evolution of close-in planets. The dependence of thetidal interactions on the structural and rotational evolution of the star is ofpeculiar importance and should be correctly treated. We quantify how tidaldissipation in the convective envelope of rotating low-mass stars evolves fromthe pre-main sequence up to the red-giant branch depending on the initialstellar mass. We investigate the consequences of this evolution on planetaryorbital evolution. We couple the tidal dissipation formalism described inMathis (2015) to the stellar evolution code STAREVOL and apply it to rotatingstars with masses between 0.3 and 1.4 M$_\odot$. In addition, we generalize thework of Bolmont & Mathis (2016) by following the orbital evolution of close-inplanets using the new tidal dissipation predictions for advanced phases ofstellar evolution. On the PMS the evolution of tidal dissipation is controlledby the evolution of the internal structure of the contracting star. On the MSit is strongly driven by the variation of surface rotation that is impacted bymagnetized stellar winds braking. The main effect of taking into account therotational evolution of the stars is to lower the tidal dissipation strength byabout four orders of magnitude on the main-sequence, compared to a normalizeddissipation rate that only takes into account structural changes. The evolutionof the dissipation strongly depends on the evolution of the internal structureand rotation of the star. From the pre-main sequence up to the tip of thered-giant branch, it varies by several orders of magnitude, with strongconsequences for the orbital evolution of close-in massive planets. Theseeffects are the strongest during the pre-main sequence, implying that theplanets are mainly sensitive to the star's early history.

astronomy and astrophysics

Tidal dissipation in rotating low-mass stars and implications for the  orbital evolution of close-in planets I. From the PMS to the RGB at solar  metallicity