Context : The lower limit to the distribution of orbital periods P for the current population of close-in exoplanets shows a distinctive discontinuity located at approximately one Jovian mass .
Most smaller planets have orbital periods longer than P \sim 2.5 days , while higher masses are found down to P \sim 1 day .

Aims : We analyze whether this observed mass-period distribution could be explained in terms of the combined effects of stellar tides and the interactions of planets with an inner cavity in the gaseous disk .

Methods : We performed a series of hydrodynamical simulations of the evolution of single-planet systems in a gaseous disk with an inner cavity mimicking the inner boundary of the disk .
The subsequent tidal evolution is analyzed assuming that orbital eccentricities are small and stellar tides are dominant .

Results : We find that most of the close-in exoplanet population is consistent with an inner edge of the protoplanetary disk being located at approximately P \gtrsim 2 days for solar-type stars , in addition to orbital decay having been caused by stellar tides with a specific tidal parameter on the order of Q ^ { \prime } _ { * } \simeq 10 ^ { 7 } .
The data is broadly consistent with planets more massive than one Jupiter mass undergoing type II migration , crossing the gap , and finally halting at the interior 2/1 mean-motion resonance with the disk edge .
Smaller planets do not open a gap in the disk and remain trapped in the cavity edge .
CoRoT-7b appears detached from the remaining exoplanet population , apparently requiring additional evolutionary effects to explain its current mass and semimajor axis .

Conclusions :