Convective Instability in Core-Collapse Supernovae

Details Convective Instability in Core-Collapse Supernovae Convective Instability in Core-Collapse Supernovae

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...197.8110s&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #81.10; Bulletin of the American Astronomical Society, Vol. 32, p.1539

Astronomy and Astrophysics

Astronomy

Scientific paper

We are investigating the effects of asymmetry on convective instability in core-collapse supernovae. We use the numerical hydrodynamics code, VH-1, to simulate the shock wave resulting from a core-bounce of a Type II (core-collapse) supernova. We perform simulations in both one and two dimensions with symmetric and various asymmetric density perturbation conditions. Simulations showed that for asymmetric conditions there are significant increases in convective instability within milliseconds after bounce with only minor density perturbations. Diagnostics include animations of entropy, angular velocity and vorticity, as well as graphical analysis of average shock radius and the kinetic energy of turbulence.

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