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We perform axisymmetric (2D) multi-angle, multi-group neutrinoradiation-hydrodynamic calculations of the postbounce phase of core-collapsesupernovae using a genuinely 2D discrete-ordinate (S_n) method. We follow thelong-term postbounce evolution of the cores of one nonrotating and onerapidly-rotating 20-solar-mass stellar model for ~400 milliseconds from 160 msto ~550 ms after bounce. We present a multi-D analysis of the multi-angleneutrino radiation fields and compare in detail with counterpart simulationscarried out in the 2D multi-group flux-limited diffusion (MGFLD) approximationto neutrino transport. We find that 2D multi-angle transport is superior incapturing the global and local radiation-field variations associated withrotation-induced and SASI-induced aspherical hydrodynamic configurations. Inthe rotating model, multi-angle transport predicts much larger asymptoticneutrino flux asymmetries with pole to equator ratios of up to ~2.5, whileMGFLD tends to sphericize the radiation fields already in the opticallysemi-transparent postshock regions. Along the poles, the multi-anglecalculation predicts a dramatic enhancement of the neutrino heating by up to afactor of 3, which alters the postbounce evolution and results in greater polarshock radii and an earlier onset of the initially rotationally weakened SASI.In the nonrotating model, differences between multi-angle and MGFLDcalculations remain small at early times when the postshock region does notdepart significantly from spherical symmetry. At later times, however, thegrowing SASI leads to large-scale asymmetries and the multi-angle calculationpredicts up to 30% higher average integral neutrino energy deposition ratesthan MGFLD.

2D Multi-Angle, Multi-Group Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores