We present four ab initio axisymmetric core-collapse supernova simulations initiated from 12 , 15 , 20 , and 25 M _ { \sun } zero-age main sequence 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 .
All four simulations were computed with our Chimera code employing spectral neutrino transport , special and general relativistic transport effects , and state-of-the-art neutrino interactions .
The first 0.5 seconds of evolution of these simulations was reported in Bruenn et al .
( 2013 ) , at which time , all four models exhibited shock revival and the development of explosions driven by neutrino energy deposition .
Continuing the evolution beyond 1 second after core bounce allows the explosions to develop more fully and the processes involved in powering the explosions to become more clearly evident .
We compute explosion energy estimates , including the negative gravitational binding energy of the stellar envelope outside the expanding shock , of 0.34 , 0.88 , 0.38 , and 0.70 Bethe ( B \equiv 10 ^ { 51 } ergs ) and increasing at 0.03 , 0.15 , 0.19 , and 0.52 { \mbox { B~ { } s } } ^ { -1 } , respectively , for the 12 , 15 , 20 , and 25 M _ { \sun } models at the endpoint of this report .
Three of the models developed pronounced prolate shock morphologies , while the 20 M _ { \sun } model , though exhibiting lobes and accretion streams like the other models , develops an approximately spherical , off-center shock as the explosion begins and then becomes moderately prolate only \sim 600 ms after bounce .
The explosion geometry of the 20 M _ { \sun } model has reduced the model ’ s explosion energy relative to the 15 and 25 M _ { \sun } models by reducing the mass accretion rate during the critical power-up phase of the explosion .
We examine the growth of the explosion energy in our models through detailed analyses of the energy sources and flows .
We compare the explosion energies and masses of ejected \mathrm { { } ^ { 56 } Ni } in these models with observations and find that the 12 and 20 M _ { \sun } models have explosion energies comparable to that of the lower range of observed explosion energies while the 15 and 25 M _ { \sun } models are within the range of observed explosion energies , particularly considering the rate at which their explosion energies are increasing at the time of this report .
The ejected \mathrm { { } ^ { 56 } Ni } masses given by our models are all within observational limits .
The proto-neutron star masses and kick velocities are also within reported limits .