Recent Kepler observations revealed an unexpected abundance of “ hot ” Earth-size to Neptune-size planets in the inner 0.02 - 0.2 AU from their parent stars . We propose that these smaller planets are the remnants of massive giant planets that migrated inward quicker than they could contract . We show that such disruptions naturally occur in the framework of the Tidal Downsizing hypothesis for planet formation . We find that the characteristic planet-star separation at which such “ hot disruptions ” occur is R \approx 0.03 - 0.2 AU . This result is independent of the planet ’ s embryo mass but is dependent on the accretion rate in the disc . At high accretion rates , \dot { M } \lower 2.15 pt \hbox { $ \buildrel > \over { \sim } $ } 10 ^ { -6 } { { M } _ { \odot } } yr ^ { -1 } , the embryo is unable to contract quickly enough and is disrupted . At late times , when the accretion rate drops to \dot { M } \lower 2.15 pt \hbox { $ \buildrel < \over { \sim } $ } 10 ^ { -8 } { { M } _ { \odot } } yr ^ { -1 } , the embryos migrate sufficiently slow to not be disrupted . These “ late arrivals ” may explain the well known population of hot jupiters . If type I migration regime is inefficient , then our model predicts a pile-up of planets at R \sim 0.1 AU as the migration rate suddenly switches from the type II to type I in that region .