  The phase-transition induced collapse of a neutron star to a more compact
configuration (typically a ``strange'' star) and the subsequent core bounce is
often invoked as a model for gamma-ray bursts. We present the results of
numerical simulations of this kind of event using realistic neutrino physics
and a high density equation of state. The nature of the collapse itself is
represented by the arbitrary motion of a piston deep within the star, but if
any shock is to develop, the transition, or at least its final stages, must
occur in less than a sonic time. Fine surface zoning is employed to adequately
represent the acceleration of the shock to relativistic speeds and to determine
the amount and energy of the ejecta. We find that these explosions are far too
baryon-rich (ejected Mass > 0.01 solar masses) and have much too low an energy
to explain gamma-ray bursts. The total energy of the ejecta having relativistic
lorentz factors > 40 is less than 10^46 erg even in our most optimistic models
(deep bounce, no neutrino losses or photodisintegration). However, the total
energy of all the ejecta, mostly mildly relativistic, is roughly 10^51 erg and,
if they occur, these events might be observed. They would also contribute to
Galactic nucleosynthesis, especially the r-process, even though the most
energetic layers are composed of helium and nucleons, not heavy elements.
