Physics
Scientific paper
Nov 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..ses.eb009u&link_type=abstract
American Physical Society, The 70th Annual Meeting of the Southeastern Section, November 6-8, 2003, Wilmington, North Carolina,
Physics
Scientific paper
We present numerical magnetohydrodynamic simulations of the effect of weak magnetic field on idealized Standing Accretion Shocks (SAS) that arise in classical core-collapse supernovae, wherein an expanding shock front stalls at a radius of order 200 km and remains quite stationary for a relatively long period of time (300 ms or more). In the models we present here, specific angular momentum is fixed at the outer boundary where outer core material is free-falling onto the stalled accretion shock. To ensure that the initial seed magnetic field has a poloidal component, a necessary condition for the possible growth of magneto-rotational instability (MRI), we use a weak dipole magnetic field. Our fully dynamical simulations of this interaction of rotation and the magnetic field in SAS in the context of core-collapse supernovae, show a substantial exponential growth of the magnetic field energy that can exceed 8 orders of magnitude, and which dominates the linear growth process of ``field-line wrapping''. This is characteristic of MRI growth in our models.
Blondin John
ud-Doula Asif
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