  Highly energetic stellar tidal disruption events (TDEs) provide a way to
study black hole characteristics and their environment. We simulate TDEs with
the PHANTOM code in a general relativistic and Newtonian description of a
supermassive black hole's gravity. Stars, which are placed on parabolic orbits
with different parameters $\beta$, are constructed with the stellar evolution
code MESA and therefore have realistic stellar density profiles. We study the
mass fallback rate of the debris $\dot{M}$ and its dependence on the $\beta$,
stellar mass and age as well as the black hole's spin and the choice of the
gravity's description. We calculate peak value $\dot{M}_\mathrm{peak}$, time to
the peak $t_\mathrm{peak}$, duration of the super-Eddington phase
$t_\mathrm{Edd}$, time $t_{>0.5\dot{M}_\mathrm{peak}}$ during which
$\dot{M}>0.5\dot{M}_\mathrm{peak}$, early rise-time $\tau_\mathrm{rise}$ and
late-time slope $n_\infty$. We recover the trends of $\dot{M}_\mathrm{peak}$,
$t_\mathrm{peak}$, $\tau_\mathrm{rise}$ and $n_\infty$ with $\beta$, stellar
mass and age, which were obtained in previous studies. We find that
$t_\mathrm{Edd}$, at a fixed $\beta$, scales primarily with the stellar mass,
while $t_{>0.5\dot{M}_\mathrm{peak}}$ scales with the compactness of stars. The
effect of SMBH's rotation depends on the orientation of its rotational axis
relative to the direction of the stellar motion on the initial orbit.
Encounters on prograde orbits result in narrower $\dot{M}$ curves with higher
$\dot{M}_\mathrm{peak}$, while the opposite occurs for retrograde orbits. We
find that disruptions, at the same pericenter distance, are stronger in a
relativistic tidal field than in a Newtonian. Therefore, relativistic $\dot{M}$
curves have higher $\dot{M}_\mathrm{peak}$, and shorter $t_\mathrm{peak}$ and
$t_\mathrm{Edd}$.
