J. Austin Harris

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

Three dimensional core-collapse supernova simulated using a 15 M⊙ progenitor

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 (

Essential ingredients in core-collapse supernovae

10^{51}

Gravitational wave signatures of ab initio two-dimensional core collapse supernova explosion models for 12 – 25 M ⊙ stars

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

Recent Progress on Ascertaining the Core Collapse Supernova Explosion Mechanism

^{-1}

The Gravitational Wave Signal of a Core Collapse Supernova Explosion of a 15 M

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

_\odot

M_\odot

Star

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

Two- and Three-Dimensional Multi-Physics Simulations of Core Collapse Supernovae: A Brief Status Report and Summary of Results from the “Oak Ridge” Group

M_\odot