  We present simulations of the tidal disruption of a solar mass star by a
$10^6M_{\odot}$ black hole. These, for the first time, cover the full time
evolution of the tidal disruption event, starting well before the initial
encounter and continuing until more than 90% of the bound material has returned
to the vicinity of the hole. Our results are compared to the analytical
prediction for the rate at which tidally-stripped gas falls back. We find that,
for our chosen parameters, the overall scaling of the fallback rate,
$\dot{M}_{\rm{fb}}$, closely follows the canonical $t^{-5/3}$ power-law.
However, our simulations also show that the self-gravity of the tidal stream,
which dominates the tidal gravity of the hole at large distances, causes some
of the debris to recollapse into bound fragments before returning to the hole.
This causes $\dot{M}_{\rm{fb}}$ to vary significantly around the $t^{-5/3}$
average. We discuss the implications of our findings in the context of the
event Swift J1644+57.
