Super-Eddington Accretion in Tidal Disruption Events: the Impact of
  Realistic Fallback Rates on Accretion Rates
  After the tidal disruption of a star by a massive black hole, disrupted
stellar debris can fall back to the hole at a rate significantly exceeding its
Eddington limit. To understand how black hole mass affects the duration of
super-Eddington accretion in tidal disruption events, we first run a suite of
simulations of the disruption of a Solar-like star by a supermassive black hole
of varying mass to directly measure the fallback rate onto the hole, and we
compare these fallback rates to the analytic predictions of the "frozen-in"
model. Then, adopting a Zero-Bernoulli Accretion flow as an analytic
prescription for the accretion flow around the hole, we investigate how the
accretion rate onto the black hole evolves with the more accurate fallback
rates calculated from the simulations. We find that numerically-simulated
fallback rates yield accretion rates onto the hole that can, depending on the
black hole mass, be nearly an order of magnitude larger than those predicted by
the frozen-in approximation. Our results place new limits on the maximum black
hole mass for which super-Eddington accretion occurs in tidal disruption
events.
