  Intermediate mass black holes (IMBHs, $\sim 10^2-10^5M_{\odot}$) are often
dubbed as the missing link between stellar mass ($\lesssim 10^2M_{\odot}$) and
super-massive ($\gtrsim 10^{5-6} M_{\odot}$) black holes. Observational
signatures of these can result from tidal disruptions of white dwarfs (WDs),
which would otherwise be captured as a whole by super-massive black holes.
Recent observations indicate that IMBHs might be rapidly spinning, while it is
also known that isolated white dwarfs might have large spins, with spin periods
of the order of minutes. Here, we aim to understand the effects of ``coupling''
between black hole and stellar spin, focussing on the tidal disruption of
spinning WDs in the background of spinning IMBHs. Using smoothed particle
hydrodynamics, we perform a suite of numerical simulations of partial tidal
disruptions, where spinning WDs are in eccentric orbits about spinning IMBHs.
We take a hybrid approach, where we integrate the Kerr geodesic equations while
being in a regime where we can treat the internal stellar fluid dynamics in the
Newtonian limit. We observe strong dependence of quantities like the core mass
and the mass differences between tidal tails on such coupled spin effects.
However, observable quantities such as mass fallback rates and gravitational
wave amplitudes show minimal variations with these, in the parameter range that
we consider.
