  More than 1500 exoplanets have been discovered around a large diversity of
host stars (from M- to A-type stars). Tidal dissipation in their convective
envelope is a key actor that shapes the orbital architecture of short-period
systems and that still remains unknown. Using a simplified two-layer assumption
and grids of stellar models, we compute analytically an equivalent modified
tidal quality factor, which is proportional to the inverse of the
frequency-averaged dissipation due to the viscous friction applied by turbulent
convection on tidal waves. It leads the conversion of their kinetic energy into
heat and tidal evolution of orbits and spin. During their Pre-Main-Sequence,
all low-mass stars have a decrease of the equivalent modified tidal quality
factor for a fixed angular velocity of their convective envelope. Next, it
evolves 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 magnitude
with increasing stellar mass. Finally, the rotational evolution of low-mass
stars strengthens tidal dissipation during the Pre-Main-Sequence.
