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

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