  We have carried out general relativistic particle simulations of stars
tidally disrupted by massive black holes. When a star is disrupted in a bound
orbit with moderate eccentricity instead of a parabolic orbit, the temporal
behavior of the resulting stellar debris changes qualitatively. The debris is
initially all bound, returning to pericenter in a short time ~ the original
stellar orbital timescale. The resulting fallback rate can thus be much higher
than the Eddington rate. Furthermore if the star is disrupted close to the
hole, in a regime where general relativity is important, the stellar and debris
orbits display general relativistic precession. Apsidal precession can make the
debris stream cross itself after several orbits, likely leading to fast debris
energy dissipation. If the star is disrupted in an inclined orbit around a
spinning hole, nodal precession reduces the probability of self-intersection,
and circularization may take many dynamical timescales, delaying the onset of
flare activity. An examination of the particle dynamics suggests that
quasi-periodic flares with short durations, produced when the center of the
tidal stream passes pericenter, may occur in the early-time light curve. The
late-time light curve may still show power-law behavior which is generic to
disk accretion processes. The detection triggers for future surveys should be
extended to capture such "non-standard" short-term flaring activity before the
event enters the asymptotic decay phase, as this activity is likely to be more
sensitive to physical parameters such as the black hole spin.
