  Through tidal dissipation in a slowly spinning host star the orbits of many
hot Jupiters may decay down to the Roche limit. We expect that in most cases
the ensuing mass transfer will be stable. Using detailed numerical calculations
we find that this evolution is quite rapid, potentially leading to complete
removal of the gaseous envelope in a few Gyr, and leaving behind an exposed
rocky core ("hot super-Earth"). Final orbital periods are quite sensitive to
the details of the planet's mass-radius relation, and to the effects of
irradiation and photo-evaporation, but could be as short as a few hours, or as
long as several days. Our scenario predicts the existence of planets with
intermediate masses ("hot Neptunes") that should be found precisely at their
Roche limit and in the process of losing mass through Roche lobe overflow. The
observed excess of small single-planet candidate systems observed by Kepler may
also be the result of this process. If so, the properties of their host stars
should track those of the hot Jupiters. Moreover, the number of systems that
produced hot Jupiters could be 2-3 times larger than one would infer from
contemporary observations.
