Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...203.4513u&link_type=abstract
American Astronomical Society Meeting 203, #45.13; Bulletin of the American Astronomical Society, Vol. 35, p.1279
Astronomy and Astrophysics
Astronomy
Scientific paper
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.
Blondin John
ud-Doula Asif
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