  In dense star clusters, such as globular and open clusters, dynamical
interactions between stars and black holes (BHs) can be extremely frequent,
leading to various astrophysical transients. Close encounters between a star
and a stellar mass BH make it possible for the star to be tidally disrupted by
the BH. Due to the relative low mass of the BH and the small cross section of
the tidal disruption event (TDE) for cases with high penetration, disruptions
caused by close encounters are usually partial disruptions. The existence of
the remnant stellar core and its non-negligible mass compared to the stellar
mass BH alters the accretion process significantly. We study this problem with
SPH simulations using the code {\tt Phantom}, with the inclusion of radiation
pressure, which is important for small mass BHs. Additionally, we develop a
new, more general method of computing the fallback rate which does not rely on
any approximation. Our study shows that the powerlaw slope of the fallback rate
has a strong dependence on the mass of the BH in the stellar mass BH regime.
Furthermore, in this regime, self-gravity of the fallback stream and local
instabilities become more significant, and cause the disrupted material to
collapse into small clumps before returning to the BH. This results in an
abrupt increase of the fallback rate, which can significantly deviate from a
powerlaw. Our results will help in the identification of TDEs by stellar mass
BHs in dense clusters.
