  Fallback rate of debris after a partial tidal disruption event of a star with
an intermediate mass black hole (IMBH) might provide important signatures of
such black holes, compared to supermassive ones. Here using smoothed particle
hydrodynamics methods, we provide a comprehensive numerical analysis of this
phenomenon. We perform numerical simulations of single partial tidal
disruptions of solar mass white dwarfs in parabolic orbits, with a non-spinning
$10^3M_{\odot}$ IMBH for various values of the impact parameter, and determine
the core mass fractions and fallback rates of debris into the IMBH. For
supermassive black holes, in a full disruption processes, it is known that the
late time fallback rate follows a power law $t^{-5/3}$, whereas for partial
disruptions, such a rate has been recently conjectured to saturate to a steeper
power law $t^{-9/4}$, independent of the mass of the remnant core. We show here
that for IMBHs, partial disruptions significantly alter this conclusion. That
is, the fallback rate at late times do not asymptote to a $t^{-9/4}$ power law,
and this rate is also a strong function of the core mass. We derive a robust
formula for the late time fallback rate as a function of the core mass
fraction, that is independent of the white dwarf mass, as we verify numerically
by varying the mass of the white dwarf.
