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The impact of the magnetic field on postbounce supernova dynamics ofnon-rotating stellar cores is studied by performing three-dimensionalmagnetohydrodynamics simulations with spectral neutrino transport. Theexplodability of strongly and weakly magnetized models of $20$ and $27$$M_{\odot}$ pre-supernova progenitors are compared. We find that although theefficiency for the conversion of the neutrino heating into turbulent energyincluding magnetic fields in the gain region is not significantly differentbetween the strong and weak field models, the amplified magnetic field due tothe neutrino-driven convection on large hot bubbles just behind stalled shockresults in a faster and more energetic explosion in the strongly magnetizedmodels. In addition, by comparing the difference between the 2nd- and 5th-orderspatial accuracy of the simulation in the strong field model for $27$$M_{\odot}$ progenitor, we also find that the higher order accuracy in space isbeneficial to the explosion because it enhances the growth of neutrino-drivenconvection in the gain region. Based on our results of core-collapse supernovasimulations for the non-rotating model, a new possibility for the origin of themagnetic field of the protoneutron star (PNS) is proposed. The magnetic fieldis accumulated and amplified to magnetar level, that is, $\mathcal{O}(10^{14})$G, in the convectively stable shell near the PNS surface.

Magnetic support for neutrino-driven explosion of 3D non-rotating core-collapse supernova models