  Since twenty years, a large population of close-in planets orbiting various
classes of low-mass stars (from M to A-type stars) has been discovered. In such
systems, the dissipation of the kinetic energy of tidal flows in the host star
may modify its rotational evolution and shape the orbital architecture of the
surrounding planetary system. In this context, recent works demonstrated that
the amplitude of this dissipation can vary over several orders of magnitude as
a function of stellar mass, age and rotation. In addition, the stellar rotation
evolution strongly impacts angular momentum exchanges within star-planet
systems. Therefore, it is now necessary to take into account the structural and
rotational evolution of stars when studying the orbital evolution of close-in
planets. The presence of planets may also modify the rotation of the host stars
and as a consequence their evolution, magnetic activity and mixing. In this
work, we present the first study of the dynamics of close-in planets of various
masses orbiting low-mass stars (from $0.6$ to $1.2~M_\star$) where we compute
the simultaneous evolution of the star's structure, rotation and tidal
dissipation in its external convective enveloppe. We find that tidal friction
due to the stellar dynamical tide, i.e. tidal inertial waves excited in the
convection zone, can be larger by several orders of magnitude than the one of
the equilibrium tide, especially during the PMS phase. Consequently, the
orbital migration of the planet is now more pronounced and depends more on the
stellar mass, rotation and age. This would very weakly affect the planets in
the habitable zone because they are located at orbital distances such that
stellar tide-induced migration happens on very long timescales. We also
demonstrate that the rotational evolution of host stars is only weakly affected
by the presence of planets except for massive companions.
