ThreeDimensional Simulations of Convection in Supernova Cores
Abstract
We have carried out threedimensional simulations of convection above the proto neutron star in supernova explosions; this convection is driven by a negative entropy gradient due to heating of shocked matter by highenergy neutrinos radiated from the proto neutron star. We compared the threedimensional calculations with axisymmetric or spherical calculations by changing the initial perturbations. We found that the explosion energy is unchanged by convective motion, but that convection can explain the seed of matter mixing. We also found that threedimensional motion has an advantage for the ejection of rprocess nuclei synthesized in hot bubbles.
 Publication:

Publications of the Astronomical Society of Japan
 Pub Date:
 August 1993
 Bibcode:
 1993PASJ...45L..53S
 Keywords:

 Computerized Simulation;
 Shock Wave Propagation;
 Stellar Convection;
 Supernovae;
 Three Dimensional Models;
 Mixing Layers (Fluids);
 Nuclear Fusion;
 Perturbation Theory;
 Three Dimensional Motion;
 Astrophysics;
 CONVECTION;
 STARS: SUPERNOVAE;
 STARS: INDIVIDUAL (SN1987A);
 MATTER MIXING;
 NUCLEOSYNTHESIS (RPROCESS)