AAS 203rd Meeting, January 2004
Session 45 Supernovae
Poster, Tuesday, January 6, 2004, 9:20am-6:30pm, Grand Hall

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[45.13] The Magneto-Rotational Instability in Standing Accretion Shocks

A. ud-Doula, J. Blondin (NCSU)

We present numerical magnetohydrodynamic (MHD) 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 ~ 100-200 km and remains quite stationary for a relatively long period of time ~ 300 ms. In the models we present here, specific angular momentum is fixed at the outer boundary. 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 order of magnitude, and which dominates the linear growth process of ``field-line wrapping''. This is characteristic of MRI growth in our models.

The author(s) of this abstract have provided an email address for comments about the abstract: auddoula@yahoo.com

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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.