Development of Convection in Post-shock Regions of Core Collapse Supernovae

Details Development of Convection in Post-shock Regions of Core Collapse Supernovae Development of Convection in Post-shock Regions of Core Collapse Supernovae

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...207.1713m&link_type=abstract

American Astronomical Society Meeting 207, #17.13; Bulletin of the American Astronomical Society, Vol. 37, p.1183

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We present results of 2-D simulations of core-collapse supernovae in the period immediately following core bounce. We have discovered the rapid onset of instabilities that quickly develop into convection in the post-shock region. Convection in this region quickly erases the driving entropy gradients, leaving behind an anemic convective zone. These high-resolution models exhibit much smaller-scale convective features than any that have been heretofore reported. We also see the development of a large scale instability that looks remarkably like the standing accretion shock instability (SASI) that was discovered by Blondin et al. However, in our current models, this SASI-like instability does not persist for any significant time.
This work was performed at the State University of New York at Stony Brook as part of the TeraScale Supernova Initiative, and is funded by SciDAC grant DE-FC02-01ER41185 from the U.S. Department of Energy, Office of Science High-Energy, Nuclear, and Advanced Scientific Computing Research Programs. We gratefully acknowledge support of the National Energy Research Scientific Computing Center (NERSC) for computational and consulting support.

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