Abstract
We performed the first numerical simulations of magnetorotational instability from a sub-magnetar-class seed magnetic field in core collapse supernovae. As a result of axisymmetric ideal MHD simulations, we found that the magnetic field is greatly amplified to magnetar-class strength. In saturation phase, a substantial part of the core is dominated by turbulence, and the magnetic field possesses dominant large scale components, comparable to the size of the proto-neutron star. A pattern of coherent chanel flows, which generally appears during exponential growth phase in previous local simulations, is not observed in our global simulations. While the approximate convergence in the exponential growth rate is attained by increasing spatial resolution, that of the saturation magnetic field is not achieved due to still large numerical diffusion. Although the effect of magnetic field on the dynamics is found to be mild, a simulation with a high-enough resolution might result in a larger impact.
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