  Tidal interactions and planet evaporation processes impact the evolution of
close-in star-planet systems. We study the impact of stellar rotation on these
processes. We compute the time evolution of star-planet systems consisting of a
planet with initial mass between 0.02 and 2.5 M$_{ Jup}$ (6 and 800 M$_{
Earth}$), in a quasi-circular orbit with an initial orbital distance between
0.01 and 0.10 au, around a solar-type star evolving from the Pre-Main-Sequence
(PMS) until the end of the Main-Sequence (MS) phase. We account for the
evolution of: the stellar structure, the stellar angular momentum due to tides
and magnetic braking, the tidal interactions (equilibrium and dynamical tides
in stellar convective zones), the mass-evaporation of the planet, and the
secular evolution of the planetary orbit. We consider that at the beginning of
the evolution, the proto-planetary disk has fully dissipated and planet
formation is complete. Both a rapid initial stellar rotation, and a more
efficient angular momentum transport inside the star, in general, contribute
toward the enlargement of the domain which is devoid of planets after the PMS
phase, in the plane of planet mass vs. orbital distance. Comparisons with the
observed distribution of exoplanets orbiting solar mass stars, in the plane of
planet mass vs. orbital distance (addressing the "Neptunian desert" feature),
show an encouraging agreement with the present simulations, especially since no
attempts have been made to fine-tune initial parameters of the models to fit
the observations. We also obtain an upper limit for the orbital period of
bare-core planets, that agrees with observations of the "radius valley" feature
in the plane of planet radius vs. orbital period. The two effects, tides and
planet evaporation, should be accounted for simultaneously and in a consistent
way, with a detailed model for the evolution of the star.
