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Paper: MHD Simulations of Non-rotating Stellar Core Collapse with Neutrinos
Volume: 459, 6th International Conference of Numerical Modeling of Space Plasma Flows (ASTRONUM 2011)
Page: 149
Authors: Obergaulinger, M.; Janka, T.
Abstract: Using a new code for the solution of the coupled equations of magnetohydrodynamics (MHD) and neutrino transport, we simulate the collapse and post-bounce evolution of the core of a non-rotating massive star endowed with a poloidal magnetic field. Our code solves the hyperbolic system of the two-moment equations for the transport of electron neutrinos and antineutrinos and the MHD equations in a finite-volume discretisation using high-resolution shock capturing methods. The coupling between the neutrinos and the gas is accounted for by the most important weak interactions. Although the absence of rotation restricts the possible mechanisms for the amplification of the magnetic field, we find a strong growth of the initial field by flux-freezing compression during collapse and by hydrodynamic instabilities afterwards. From an initial field comparable to the results of current stellar-evolution calculations, the core reaches a field strength in the range observed typically at the surface of pulsars, while a much stronger initial field gives rise to magnetar-like final fields.
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