  We present a numerical investigation of the tidal disruption of white dwarfs
by moderately massive black holes, with particular reference to the centers of
dwarf galaxies and globular clusters. Special attention is given to the fate of
white dwarfs of all masses that approach the black hole close enough to be
disrupted and severely compressed to such extent that explosive nuclear burning
can be triggered. Consistent modeling of the gas dynamics together with the
nuclear reactions allows for a realistic determination of the explosive energy
release. In the most favorable cases, the nuclear energy release may be
comparable to that of typical type Ia supernovae. Although the explosion will
increase the mass fraction escaping on hyperbolic orbits, a good fraction of
the debris remains to be swallowed by the hole, causing a bright soft X-ray
flare lasting for about a year. Such transient signatures, if detected, would
be a compelling testimony for the presence of a moderately mass black hole
(below $10^5 M_\odot$).
