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According to the traditional scenario for core-collapse supernovae, the coreof the collapsing star forms a neutron star and its gravitational energyrelease sends out a shockwave into the stellar envelope. However, in asignificant number of numerical simulations, the shock stalls and the starcannot be exploded successfully, especially for a massive, compact star. Weconsider an alternative scenario that with mass fallback, the collapsing starforms a black hole in the center, surrounded by a dense, hot accretion disk,which blows out an intense outflow (wind). The kinetic energy of the wind mayresult in a successful stellar explosion. With an improved version of theformulism in Kohri et al. (2005) who studied neutron star accretion of minorfallback, we study this disk wind-driven explosion by calculating the accretionhistory for a suite of pre-SN stellar models with different initial surfacerotational velocities, masses and metallicities, and by comparing the disk windenergy with the binding energy of the infalling stellar envelope. We show thatthe most promising models to be exploded successfully by this new channel arethose relatively compact pre-SN stars with relatively low metallicities and nottoo low specific angular momenta. The total energies of the explosions are$\sim 10^{51-52}$ergs, and a more massive progenitor may produce a moreenergetic explosion.

Mechanical feedback from black hole accretion as an energy source of core-collapse supernova explosions