  We compute the possible observational signatures of white dwarf dynamical
interactions in dense stellar environments. Specifically, we compute the
emission of gravitational waves, and we compare it with the sensitivity curves
of planned space-borne gravitational wave detectors. We also compute the light
curves for those interactions in which a detonation occurs, and one of the
stars is destroyed, as well as the corresponding neutrino luminosities. We find
that for the three possible outcomes of these interactions - which are the
formation of an eccentric binary system, a lateral collision in which several
mass transfer episodes occur, and a direct one in which just a single mass
transfer episode takes place - only those in which an eccentric binary are
formed are likely to be detected by the planned gravitational wave mission
eLISA, while more sensitive detectors would be able to detect the signals
emitted in lateral collisions. On the other hand, the light curves (and the
thermal neutrino emission) of these interactions are considerably different,
producing both very powerful outbursts and low luminosity events. Finally, we
also calculate the X-ray signature produced in the aftermath of those
interactions for which a merger occurs. We find that the temporal evolution
follows a power law with the same exponent found in the case of the mergers of
two neutron stars, although the total energy released is smaller.
