  The tidal disruption of stars by (super-)massive black holes in galactic
nuclei has been discussed in theoretical terms for about 30 years but only in
the past decade have we been able to detect such events in substantial numbers.
Thus, we are now starting to carry out observational tests of models for the
disruption. We are also formulating expectations for the inspiral and
disruption of white dwarfs by intermediate-mass black holes with masses $<
10^5\;{\rm M}_\odot$. Such events are very rich with information and open a new
window to intermediate-mass black holes, thought to live in dwarf galaxies and
star clusters. They can inform us of the demographics of intermediate-mass
black holes, stellar populations and dynamics in their immediate vicinity, and
the physics of accretion of hydrogen-deficient material. The combination of
upcoming transient surveys using ground-based, electromagnetic observatories
and low-frequency gravitational wave observations is ideal for exploiting tidal
disruptions of white dwarfs. The detection rate of gravitational wave signals,
optimistically, may reach a few dozen per year in a volume up to $z\approx
0.1$. Gravitational wave observations are particularly useful because they
yield the masses of the objects involved and allow determination of the spin of
the black hole, affording tests of physical models for black hole formation and
growth. They also give us advance warning of the electromagnetic flares by
weeks or more. The right computing infrastructure for modern models for the
disruption process and event rates will allow us to make the most of the
upcoming observing facilities.
