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The final collapse of the cores of massive stars can lead to a wide varietyof outcomes in terms of electromagnetic and kinetic energies, nucleosynthesis,and remnants. The connection of this wide spectrum of explosion and remnanttypes to the properties of the progenitors remains an open issue. Rotation andmagnetic fields in Wolf-Rayet stars of subsolar metallicity may explain extremeevents such as superluminous supernovae and gamma-ray bursts powered byproto-magnetars or collapsars. Continuing numerical studies ofmagnetorotational core collapse including detailed neutrino physics, we focuson progenitors with zero-age main-sequence masses in the range between 5 and 39solar masses. The pre-collapse stars are one dimensional models employingprescriptions for the effects of rotation and magnetic fields. Eight of the tenstars we consider being the results of chemically homogeneous evolution due toenhanced rotational mixing (Aguilera-Dena et al. 2018). All but one of themproduce explosions driven by neutrino heating (more likely for low massprogenitors up to 8 solar masses) and non-spherical flows or bymagnetorotational stresses (more frequent above 26 solar masses). In most ofthem and for the one non-exploding model, ongoing accretion leads to black-holeformation. Rapid rotation makes a subsequent collapsar activity plausible.Models not forming black holes show proto-magnetar driven jets. Conditions forthe formation of nickel are more favourable in magneto-rotationally drivenmodels, though our rough estimates fall short of the requirements for extremelybright events if these are powered by radioactive decay. However, approximatelight curves of our models suggest that a proto-magnetar or black holespin-down may fuel luminous transients (with peak luminosities ~ 10^{43...44}erg).

Magnetorotational core collapse of possible GRB progenitors. IV. A wider range of progenitors