  A massive black hole (MBH) in a galactic center drives a flow of stars into
nearly radial orbits to replace those it destroyed. Stars whose orbits cross
the event horizon r_s or the tidal disruption radius r_t are promptly destroyed
in an orbital period P. Stars with orbital periapse r_p slightly larger than
the sink radius q=max(r_s,r_t) may slowly spiral in due to dissipative
interactions with the MBH, e.g. gravitational wave emission, tidal heating or
accretion disk drag, with observable consequences and implications for the MBH
growth rate. Unlike prompt destruction, the inspiral time is typically >>P.
This time is limited by the same scattering process that initially deflected
the star into its eccentric orbit, since it can deflect it again to a wider
orbit where dissipation is inefficient. The ratio between slow and prompt event
rates is therefore much smaller than that implied by the ratio of
cross-sections, ~r_p/q, and so only prompt disruption contributes significantly
to the mass of the MBH. Conversely, most stars that scatter off the MBH survive
the extreme tidal interaction ("tidal scattering"). We derive general
expressions for the inspiral event rate and the mean number of inspiraling
stars, and show that the survival probability of tidally scattered stars is ~1,
and that the number of tidally heated stars ("squeezars") and gravity wave
emitting stars in the Galactic Center is ~0.1-1.
