  In the centers of dense star clusters, close encounters between stars and
compact objects are likely to occur. We study tidal disruption events of
main-sequence (MS) stars by stellar-mass black holes (termed $\mu$TDEs), which
can shed light on the processes occurring in these clusters, including being an
avenue in the mass growth of stellar-mass BHs. Using the moving-mesh
hydrodynamics code \texttt{AREPO}, we perform a suite of hydrodynamics
simulations of partial $\mu$TDEs of realistic, \texttt{MESA}-generated MS stars
by varying the initial mass of the star ($0.5\,{\rm M}_{\rm \odot}$ and
$1\,{\rm M}_{\rm \odot}$), the age of the star (zero-age, middle-age and
terminal-age), the mass of the black hole ($10\,{\rm M}_{\rm \odot}$ and
$40\,{\rm M}_{\rm \odot}$) and the impact parameter (yielding almost no mass
loss to full disruption). We then examine the dependence of the masses, spins,
and orbital parameters of the partially disrupted remnant on the initial
encounter parameters. We find that the mass lost from a star decreases
exponentially with increasing distance of approach and that a $1\,{\rm M}_{\rm
\odot}$ star loses lesser mass than a $0.5\,{\rm M}_{\rm \odot}$. Moreover, a
more evolved star is less susceptible to mass loss. Tidal torques at the
closest approach spin up the remnant by factors of $10^2$--$10^4$ depending on
the impact parameter. The remnant star can be bound (eccentric) or unbound
(hyperbolic) to the black hole: hyperbolic orbits occur when the star's central
density concentration is relatively low and the black hole-star mass ratio is
high, which is the case for the disruption of a $0.5\,{\rm M}_{\rm \odot}$
star. Finally, we provide best-fit analytical formulae for a range of
parameters that can be incorporated into cluster codes to model star-black hole
interaction more accurately.
