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We consider accretion onto newborn black holes following the collapse ofrotating massive stellar cores, at the threshold where a centrifugallysupported disk gives way to nearly radial inflow for low angular momentum. Forrealistic initial conditions taken from pre-supernova (pre-SN) evolutioncalculations, the densities and temperatures involved require the use of adetailed equation of state and neutrino cooling processes, as well as aqualitative consideration of the effects of general relativity. Throughtwo-dimensional dynamical calculations we show how the energy release isaffected by the rotation rate and the strength of angular momentum transport,giving rise to qualitatively different solutions in limits of high and lowangular momentum, each being capable of powering a gamma-ray burst (GRB). Weexplore the likelihood of producing Fe-group elements in the two regimes andsuggest that while large and massive centrifugally supported disks are capableof driving strong outflows with a possible SN-like signature, quasi-radialflows lack such a feature and may produce a GRB without such an accompanyingfeature, as seen in GRB060505.

Gamma Ray Burst Production and Supernova Signatures in Slowly Rotating Collapsars