  Over the last two decades, a large population of close-in planets has been
detected around a wide variety of host stars. Such exoplanets are likely to
undergo planetary migration through magnetic and tidal interactions. We aim to
follow the orbital evolution of a planet along the structural and rotational
evolution of its host star by taking into account simultaneously tidal and
magnetic torques, in order to explain some properties of the distribution of
observed close-in planets. We rely on a numerical model of a coplanar circular
star-planet system taking into account stellar structural changes, wind braking
and star-planet interactions, called ESPEM. We browse the parameter space of
star-planet systems' configurations and assess the relative influence of
magnetic and tidal torques on secular evolution. We then synthesize star-planet
populations and confront their distribution in orbital and stellar rotation
periods to Kepler satellite data. First, we find that after the dissipation of
the protoplanetary disk, both types of interactions can dominate secular
evolution depending on the initial configuration of the system and the
evolutionary phase considered. Moreover, different populations of star-planet
systems emerge from the combined action of both kinds of interactions,
according to the evolutionary phase during which the planet migrates
significantly. This may affect significantly the detectability of star-planet
systems as well as the validity of gyrochonology. All in all, star-planet
interactions significantly impact the global distribution in orbital periods
during the main sequence, while the global distribution in stellar rotation
periods is marginally affected. More precisely, star-planet magnetic
interactions significantly affect the distribution of super-Earths around
slowly rotating stars, while tidal effects are found to shape the distribution
of giant planets.
