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More than 1500 exoplanets have been discovered around a large diversity ofhost stars (from M- to A-type stars). Tidal dissipation in their convectiveenvelope is a key actor that shapes the orbital architecture of short-periodsystems and that still remains unknown. Using a simplified two-layer assumptionand grids of stellar models, we compute analytically an equivalent modifiedtidal quality factor, which is proportional to the inverse of thefrequency-averaged dissipation due to the viscous friction applied by turbulentconvection on tidal waves. It leads the conversion of their kinetic energy intoheat and tidal evolution of orbits and spin. During their Pre-Main-Sequence,all low-mass stars have a decrease of the equivalent modified tidal qualityfactor for a fixed angular velocity of their convective envelope. Next, itevolves on the Main Sequence to an asymptotic value that is minimum for$0.6M_{\odot}$ K-type stars and that increases by several orders of magnitudewith increasing stellar mass. Finally, the rotational evolution of low-massstars strengthens tidal dissipation during the Pre-Main-Sequence.

The variation of the tidal quality factor of convective envelopes of rotating low-mass stars along their evolution