The characteristics of the initial magnetic field present in a supernova progenitor prior to collapse and the dynamics of the field amplification due to different dynamo mechanisms (such as MRI, convective motions, etc.) are to this date quite uncertain.
We investigate the effects of multipolar magnetic field topologies of different radial extents on the dynamics of core-collapse supernovae and the properties of the forming proto-neutron star (PNS). Using axisymmetric relativistic MHD simulations, we find that higher multipolar magnetic configurations lead to generally less energetic explosions, with the central PNS increasing its spin and becoming more massive. Models with a low order multipolar configuration tend to produce more oblate PNS which in some cases are surrounded by a rotationally supported toroidal structure. This change is the PNS shape can be directly associated with higher neutrino luminosities along the equatorial plane but smaller along the poles.