  We present an overview of two-dimensional (2D) core-collapse supernova
simulations employing neutrino transport scheme by the isotropic diffusion
source approximation. We study 101 solar-metallicity, 247 ultra metal-poor, and
30 zero-metal progenitors covering zero-age main sequence mass from $10.8
M_{\odot} $ to $75.0 M_{\odot} $. Using the 378 progenitors in total, we
systematically investigate how the differences in the structures of these
multiple progenitors impact the hydrodynamics evolution. By following a
long-term evolution over 1.0 s after bounce, most of the computed models
exhibit neutrino-driven revival of the stalled bounce shock at $\sim$ 200 - 800
ms postbounce, leading to the possibility of explosion. Pushing the boundaries
of expectations in previous one-dimensional (1D) studies, our results confirm
that the compactness parameter $\xi$ that characterizes the structure of the
progenitors is also a key in 2D to diagnose the properties of neutrino-driven
explosions. Models with high $\xi$ undergo high ram pressure from the accreting
matter onto the stalled shock, which affects the subsequent evolution of the
shock expansion and the mass of the protoneutron star under the influence of
neutrino-driven convection and the standing accretion-shock instability. We
show that the accretion luminosity becomes higher for models with high $\xi$,
which makes the growth rate of the diagnostic explosion energy higher and the
synthesized nickel mass bigger. We find that these explosion characteristics
tend to show a monotonic increase as a function of the compactness parameter
$\xi$.

High Energy Astrophysical Phenomena