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Using axisymmetric simulations coupling special relativistic MHD, anapproximate post-Newtonian gravitational potential and two-moment neutrinotransport, we show different paths for the formation of either protomagnetarsor stellar mass black holes. The fraction of prototypical stellar cores whichshould result in collapsars depends on a combination of several factors, amongwhich the structure of the progenitor star and the profile of specific angularmomentum are probably the foremost. Along with the implosion of the stellarcore, we also obtain supernova-like explosions driven by neutrino heating andhydrodynamic instabilities or by magneto-rotational effects in cores ofhigh-mass stars. In the latter case, highly collimated, mildly relativisticoutflows are generated. We find that after a rather long post-collapse phase(lasting >~ 1 sec) black holes may form in cases both of successful and failedsupernovalike explosions. A basic trend is that cores with a specific angularmomentum smaller than that obtained by standard, one-dimensional stellarevolution calculations form black holes (and eventually collapsars).Complementary, protomagnetars result from stellar cores with the standarddistribution of specific angular momentum obtained from prototypical stellarevolution calculations including magnetic torques and moderate to large massloss rates.

Protomagnetar and black hole formation in high-mass stars