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We explore the influence of non-axisymmetric modes on the dynamics of thecollapsed core of rotating, magnetized high-mass stars in three-dimensionalsimulations of a rapidly rotating star with an initial mass of $M_{ZAMS}$ = 35solar masses endowed with four different pre-collapse configurations of themagnetic field, ranging from moderate to very strong field strength andincluding the field predicted by the stellar evolution model. The model withthe weakest magnetic field achieves shock revival due to neutrino heating in again layer characterized by a large-scale, hydrodynamic m = 1 spiral mode.Later on, the growing magnetic field of the proto-neutron star launches weakoutflows into the early ejecta. Their orientation follows the evolution of therotational axis of the proto-neutron star, which starts to tilt from theoriginal orientation due to the asymmetric accretion flows impinging on itssurface. The models with stronger magnetization generate mildly relativistic,magnetically driven polar outflows propagating over a distance of $10^4$ kmwithin a few 100 ms. These jets are stabilized against disruptivenon-axisymmetric instabilities by their fast propagation and by the shear oftheir toroidal magnetic field. Within the simulation times of around 1 s, theexplosions reach moderate energies and the growth of the proto-neutron starmasses ceases at values substantially below the threshold for black holeformation, which, in combination with the high rotational energies, mightsuggest a possible later proto-magnetar activity.

Magnetorotational core collapse of possible GRB progenitors. III. Three-dimensional models