http://arxiv.org/abs/2202.07967
The impact of the magnetic field on the postbounce supernova dynamics of non-rotating stellar cores is studied by performing three-dimensional magnetohydrodynamics simulations with spectral neutrino transport. We compare the explodability between initially strongly and weakly magnetized models of $20$ and $27$ $M_{\odot}$ pre-supernova progenitors. We find that although the efficiency for the conversion of the neutrino heating into the turbulent energy including magnetic fields in the gain region is not significantly different between the strong and weak field models, the amplified magnetic field due to the neutrino-driven convection on large hot bubbles just behind a stalled shock leads to the faster and more energetic explosion in the strongly magnetized models. In addition, by comparing the difference between 2nd- and 5th-order spatial accuracy of the simulation in the strong field model for $27$ $M_{\odot}$ progenitor, we also find that the higher-order accuracy in space is positive for the explosion because it enhances the growth of neutrino-driven convection in the gain region. A new possibility of the origin of the magnetic field of the proto-neutron star (PNS) is proposed based on our results of core-collapse supernova simulations for the non-rotating model. The magnetic field is accumulated and amplified to the magnetar level, that is, $\mathcal{O}(10^{14})$ G, in the convectively stable shell in the vicinity of the PNS surface.
J. Matsumoto, Y. Asahina, T. Takiwaki, et. al.
Thu, 17 Feb 22
35/60
Comments: 15 pages, 20 figures, submitted to MNRAS
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