  The transit method is a promising means to detect exomoons, but few
candidates have been identified. For planets close to their stars, the
dynamical interaction between a satellite's orbit and the star must be
important in their evolution. Satellites beyond synchronous orbit spiral out
due to the tide raised on their planet, and it has been assumed that they would
likely escape the Hill sphere. Here we follow the evolution with a three-body
code that accounts for tidal dissipation within both the planet and the
satellite. We show that tidal dissipation in satellites often keeps them bound
to their planet, making exomoons more observable than previously thought. The
probability of escape depends on the ratio of tidal quality factors of the
planet and satellite; when this ratio exceeds 0.5, escape is usually avoided.
Instead, the satellite moves to an equilibrium in which the spin angular
momentum of the planet is not transferred into the orbit of the satellite, but
is transferred into the orbit of the planet itself. While the planet continues
spinning faster than the satellite orbits, the satellite maintains a semi-major
axis of approximately 0.41 Hill radii. These states are accompanied with modest
satellite eccentricity near 0.1 and are found to be stable over long
timescales.
