Merek A. Chertkow

The development of explosions in axisymmetric ab initio core-collapse supernova simulations of 12–25 M⊙ stars

We present four ab initio axisymmetric core-collapse supernova simulations for 12, 15, 20, and 25

Gravitational waves from core collapse supernovae

M_\odot

Multicore and accelerator development for a leadership-class stellar astrophysics code

progenitors. All of the simulations yield explosions and have been evolved for at least 1.2 seconds after core bounce and 1 second after material first becomes unbound. Simulations were computed with our Chimera code employing spectral neutrino transport, special and general relativistic transport effects, and state-of-the-art neutrino interactions. Continuing the evolution beyond 1 second allows explosions to develop more fully and the processes powering the explosions to become more clearly evident. We compute explosion energy estimates, including the binding energy of the stellar envelope outside the shock, of 0.34, 0.88, 0.38, and 0.70 B (

Implications for Post-processing Nucleosynthesis of Core-collapse Supernova Models with Lagrangian Particles

10^{51}

Advancements in Modeling Self-Consistent Core-Collapse Supernovae with CHIMERA

ergs) and increasing at 0.03, 0.15, 0.19, and 0.52 B s

Core-collapse Supernovae

^{-1}

Core-collapse supernova simulations with CHIMERA

, respectively, for the 12, 15, 20, and 25

Recent Progress on Ascertaining the Core Collapse Supernova Explosion Mechanism

M_\odot

Advancing Nucleosynthesis in Self-consistent, Multidimensional Models of Core-Collapse Supernovae

models. Three models developed pronounced prolate shock morphologies, while the 20

Chimera: A massively parallel code for core-collapse supernova simulation.

M_\odot