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The neutrino mechanism of core-collapse supernova is investigated vianon-relativistic, two-dimensional (2D), neutrino radiation-hydrodynamicsimulations. For the transport of electron flavor neutrinos, we use theinteraction rates defined by Bruenn (1985) and the isotropic diffusion sourceapproximation (IDSA) scheme, which decomposes the transported particles intotrapped particle and streaming particle components. Heavy neutrinos aredescribed by a leakage scheme. Unlike the "ray-by-ray" approach in some othermulti-dimensional supernova models, we use cylindrical coordinates and solvethe trapped particle component in multiple dimensions, improving theproto-neutron star resolution and the neutrino transport in angular andtemporal directions. We provide an IDSA verification by performing 1D and 2Dsimulations with 15 and 20 $M_\odot$ progenitors from Woosley et al.~(2007) anddiscuss the difference of our IDSA results with those existing in theliterature. Additionally, we perform Newtonian 1D and 2D simulations fromprebounce core collapse to several hundred milliseconds postbounce with 11, 15,21, and 27 $M_\odot$ progenitors from Woosley et al.~(2002) with the HS(DD2)equation of state. General relativistic effects are neglected. We obtain robustexplosions with diagnostic energies $E_{\rm dig} \gtrsim 0.1- 0.5$~B for allconsidered 2D models within approximately $100-300$ milliseconds after bounceand find that explosions are mostly dominated by the neutrino-drivenconvection, although standing accretion shock instabilities are observed aswell. We also find that the level of electron deleptonization during collapsedramatically affect the postbounce evolution, e.g.~the ignorance ofneutrino-electron scattering during collapse will lead to a stronger explosion.

Two-Dimensional Core-Collapse Supernova Simulations with the Isotropic Diffusion Source Approximation for Neutrino Transport