  The neutrino mechanism of core-collapse supernova is investigated via
non-relativistic, two-dimensional (2D), neutrino radiation-hydrodynamic
simulations. For the transport of electron flavor neutrinos, we use the
interaction rates defined by Bruenn (1985) and the isotropic diffusion source
approximation (IDSA) scheme, which decomposes the transported particles into
trapped particle and streaming particle components. Heavy neutrinos are
described by a leakage scheme. Unlike the "ray-by-ray" approach in some other
multi-dimensional supernova models, we use cylindrical coordinates and solve
the trapped particle component in multiple dimensions, improving the
proto-neutron star resolution and the neutrino transport in angular and
temporal directions. We provide an IDSA verification by performing 1D and 2D
simulations with 15 and 20 $M_\odot$ progenitors from Woosley et al.~(2007) and
discuss the difference of our IDSA results with those existing in the
literature. Additionally, we perform Newtonian 1D and 2D simulations from
prebounce 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 robust
explosions with diagnostic energies $E_{\rm dig} \gtrsim 0.1- 0.5$~B for all
considered 2D models within approximately $100-300$ milliseconds after bounce
and find that explosions are mostly dominated by the neutrino-driven
convection, although standing accretion shock instabilities are observed as
well. We also find that the level of electron deleptonization during collapse
dramatically affect the postbounce evolution, e.g.~the ignorance of
neutrino-electron scattering during collapse will lead to a stronger explosion.
