  By implementing widely-used equations of state (EOS) from Lattimer & Swesty
(LS) and H. Shen et al. (SHEN) in core-collapse supernova simulations, we
explore possible impacts of these EOS on the post-bounce dynamics prior to the
onset of neutrino-driven explosions. Our spherically symmetric (1D) and axially
symmetric (2D) models are based on neutrino radiation hydrodynamics including
spectral transport, which is solved by the isotropic diffusion source
approximation. We confirm that in 1D simulations neutrino-driven explosions
cannot be obtained for any of the employed EOS. Impacts of the EOS on the
post-bounce hydrodynamics are more clearly visible in 2D simulations. In 2D
models of a 15 M_sun progenitor using the LS EOS, the stalled bounce shock
expands to increasingly larger radii, which is not the case using the SHEN EOS.
Keeping in mind that the omission of the energy drain by heavy-lepton neutrinos
in the present scheme could facilitate explosions, we find that 2D models of an
11.2 M_sun progenitor produce neutrino-driven explosions for all the EOS under
investigation. Models using the LS EOS are slightly more energetic compared to
those with the SHEN EOS. The more efficient neutrino heating in the LS models
coincides with a higher electron antineutrino luminosity and a larger mass that
is enclosed within the gain region. The models based on the LS EOS also show a
more vigorous and aspherical downflow of accreting matter to the surface of the
protoneutron star (PNS). The accretion pattern is essential for the production
and strength of outgoing pressure waves, that can push in turn the shock to
larger radii and provide more favorable conditions for the explosion.
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