A comparison of Boltzmann and multigroup flux-limited diffusion neutrino transport during the postbounce shock reheating phase in core-collapse supernovae

We compare Newtonian three-flavor multigroup Boltzmann (MGBT) and (Bruenn's ) multigroup flux-limited diffusion (MGFLD) neutrino transport in postbounc e core-collapse supernova environments. We focus our study on quantities ce ntral to the postbounce neutrino heating mechanism for reviving the stalled shock. Stationary-state three-flavor neutrino distributions are developed in thermally and hydrodynamically frozen time slices obtained from core col lapse and bounce simulations that implement Lagrangian hydrodynamics and MG FLD neutrino transport. We obtain distributions for time slices at 106 and 233 ms after core bounce for the core of a 15 M. progenitor, and at 156 ms after core bounce for a 25 M. progenitor. For both transport methods, the e lectron neutrino and antineutrino luminosities, rms energies, and mean inve rse flux factors, all of which enter the neutrino heating rates, are comput ed as functions of radius and compared. The net neutrino heating rates are also computed as functions of radius and compared. Notably, we find signifi cant differences in neutrino luminosities and mean inverse flux factors bet ween the two transport methods for both precollapse models and for all thre e time slices. In each case, the luminosities for each transport method beg in to diverge above the neutrinospheres, where the MGBT luminosities become larger than their MGFLD counterparts, finally settling to a constant diffe rence maintained to the edge of the core. We find that the mean inverse flu x factors, which describe the degree of forward peaking in the neutrino rad iation held, also differ significantly between the two transport methods, w ith MGBT providing more isotropic radiation fields in the gain region. Most important, for a region above the gain radius we find net heating rates fo r MGBT that are as much as similar to 2 times the corresponding MGFLD rates , and we find net cooling rates below the gain radius that are typically si milar to 0.8 times the MGFLD rates. These differences stem from differences in the neutrino luminosities and mean inverse flux factors, which can be a s much as 11% and 24%, respectively. They are greatest at earlier postbounc e times for a given progenitor mass and, for a given postbounce time, great er for greater progenitor mass. We discuss the ramifications that these new results have for the supernova mechanism.