Eirik Endeve

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

TURBULENT MAGNETIC FIELD AMPLIFICATION FROM SPIRAL SASI MODES: IMPLICATIONS FOR CORE-COLLAPSE SUPERNOVAE AND PROTO-NEUTRON STAR MAGNETIZATION

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 (

Generation of Magnetic Fields By the Stationary Accretion Shock Instability

10^{51}

Helmet Streamers Gone Unstable: Two-Fluid Magnetohydrodynamic Models of the Solar Corona

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

Two-dimensional Magnetohydrodynamic Models of the Solar Corona: Mass Loss from the Streamer Belt

^{-1}

Conservative 3 + 1 general relativistic Boltzmann equation

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

Conservative 3+1 general relativistic variable Eddington tensor radiation transport equations

M_\odot

Coronal heating and solar wind acceleration; gyrotropic electron-proton solar wind

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

GENASIS: GENERAL ASTROPHYSICAL SIMULATION SYSTEM. I. REFINABLE MESH AND NONRELATIVISTIC HYDRODYNAMICS

M_\odot