  Neutrinos from core collapse supernovae can be emitted from a rapidly
accreting disk surrounding a black hole, instead of the canonical proto-neutron
star. For Galactic events, detector count rates are considerable and in fact
can be in the thousands for Super-Kamiokande. The rate of occurrence of these
accreting disks in the Galaxy is predicted to be on the order of 10^-5 yr^-1,
yet there is little observational evidence to provide an upper limit on their
formation rate. It would therefore be useful to discriminate between neutrinos
which have been produced in a proto-neutron star and those which have been
produced accretion disks. In order to distinguish between the two scenarios,
either the time profile of the neutrino luminosity or the relative fluxes of
different neutrino flavors may be considered. There are some signals that would
clearly point to one scenario or the other.
