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We study the effects of the magnetic field on the dynamics of non-rotatingstellar cores by performing two-dimensional (2D), magnetohydrodynamics (MHD)simulations. To this end, we have updated our neutrino-radiation-hydrodynamicssupernova code to include MHD employing a divergence cleaning method with bothcareful treatments of finite volume and area reconstructions. By changing theinitial strength of the magnetic field, the evolution of $15.0$, $18.4$ and$27.0$ $M_\odot$ presupernova progenitors is investigated. An intriguingfinding in our study is that the neutrino-driven explosion occurs regardless ofthe strength of the initial magnetic field. For the 2D models presented in thiswork, the neutrino heating is the main driver for the explosion, whereas themagnetic field secondary contributes to the pre-explosion dynamics. Our resultsshow that the strong magnetic field weakens the growth of the neutrino-driventurbulence in the small scale compared to the weak magnetic field. This resultsin the slower increase of the turbulent kinetic energy in the postshock region,leading to the slightly delayed onset of the shock revival for models with thestronger initial magnetic field.

Two-dimensional numerical study for magnetic field dependence of neutrino-driven core-collapse supernova models