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S. Shaw, J. M. Blondin (North Carolina State University)
Recent three-dimensional simulations of core-collapse supernovae have revealed the existence of non-axisymmetric modes of the Spherical Accretion Shock Instability, or SASI. Here we investigate the growth of these modes using two-dimensional simulations of the accretion flow in the equatorial plane of a core-collapse supernova. By perturbing a steady-state model we are able to excite both one- and two-armed spiral modes that grow exponentially with time, demonstrating that these are linearly unstable modes. By tracking the distribution of angular momentum, we demonstrate that these modes are able to efficiently separate the angular momentum of the accretion flow (which maintains a net angular momentum of zero), leading to a gradual spin-up of the underlying accreting proto-neutron star.
This work was performed under the auspices of the TeraScale Supernova Initiative, funded by SciDAC grants from the DOE Office of Science High-Energy, Nuclear, and Advanced Scientific Computing Research Programs.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.