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Paper: Magnetic Field Amplification in Non-Rotating Stellar Core Collapse
Volume: 498, Numerical Modeling of Space Plasma Flows ASTRONUM-2014
Page: 115
Authors: Obergaulinger, M.; Janka, H.-T.; Aloy, M. A.
Abstract: We study the field amplification processes in non-rotating stellar cores in axisymmetric simulations with two-moment neutrino transport. Flux-freezing in the radial infall compresses the magnetic field and contributes most to the amplification. Furthermore, convection in the proto-neutron star (PNS) and convection and the standing accretion shock instability in the hot-bubble region between the proto-neutron star and the stalled shock wave amplify the field further. Flux expulsion from the PNS convection zone leads to a layer of enhanced magnetic flux around the PNS. In the hot-bubble layer, the magnetic field is amplified on the typical time and length scales of the hydrodynamic instabilities. Very strong magnetic fields react back on the instabilities, generating large, persistent bubbles, which aid the shock revival and lead to earlier explosion.
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