  We study close encounters of a $1\,M_{\odot}$ middle-age main-sequence star
(modeled using MESA) with massive black holes through hydrodynamic simulations,
and explore in particular the dependence of the outcomes on the black hole
mass. We consider here black holes in the intermediate-mass range, $M_{\rm BH}=
100-10^4\,M_{\odot}$. Possible outcomes vary from a small tidal perturbation
for weak encounters all the way to partial or full disruption for stronger
encounters. We find that stronger encounters lead to increased mass loss at the
first pericenter passage, in many cases ejecting the partially disrupted star
on an unbound orbit. For encounters that initially produce a bound system, with
only partial stripping of the star, the fraction of mass stripped from the star
increases with each subsequent pericenter passage and a stellar remnant of
finite mass is ultimately ejected in all cases. The critical penetration depth
that separates bound and unbound remnants has a dependence on the black hole
mass when $M_{\rm BH} \lesssim 10^3\,M_{\odot}$. We also find that the number
of successive close passages before ejection decreases as we go from the
stellar-mass black hole to the intermediate-mass black hole regime. For
instance, after an initial encounter right at the classical tidal disruption
limit, a $1\,M_{\odot}$ star undergoes 16 (5) pericenter passages before
ejection from a $10\,M_{\odot}$ ($100\,M_{\odot}$) black hole. Observations of
periodic flares from these repeated close passages could in principle indicate
signatures of a partial tidal disruption event.
