Two- and three-dimensional simulations of core-collapse supernovae with CHIMERA

Abstract

Ascertaining the core-collapse supernova mechanism is a complex, and yet unsolved, problem dependent on the interaction of general relativity, hydrodynamics, neutrino transport, neutrinomatter interactions, and nuclear equations of state and reaction kinetics. Ab initio modeling of core-collapse supernovae and their nucleosynthetic outcomes requires care in the coupling and approximations of the physical components. We have built our multi-physics CHIMERA code for supernova modeling in 1-, 2-, and 3-D, using ray-by-ray neutrino transport, approximate general relativity, and detailed neutrino and nuclear physics. We discuss some early results from our current series of exploding 2D simulations and our work to perform computationally tractable simulations in 3D using the "Yin-Yang" grid.

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

“…(See animated Figure 3 for additional examples.) The dynamic behavior of the accretion shock has not received the attention afforded the SASI and convection, but previous analyses using tracer particles from CHIMERA simulations has shown that much of the matter passing through the shock is directed toward the proto-NS in accretion streams (Chertkow et al 2012;Lentz et al 2012a). We notethat the one or two accretion streams that dominate the accretion in 2D simulations is not characteristic of 3D simulations, which exhibit more numerous but weaker accretion streams Tamborra et al 2013Tamborra et al , 2014Takiwaki et al 2014;Tamborra et al 2014;Abdikamalov et al 2015;Lentz et al 2015).…”