Core-collapse supernovae (CCSNe) are an important link in the chain of stellar evolution and critically contribute to the chemical enrichment of the Universe.
Numerical modeling of CCSNe remains a challenge due to the inherent multidimensional and multi-physics nature of the problem and the diversity of initial conditions; yet, recent progress has resulted 3D simulations with detailed physics at reasonable resolutions.
We present recent results from 3D simulations that examine resolution and progenitor diversity computed with our detailed "Chimera" code.
A low-mass, zero-metal star with low density envelope explodes easily with behaviors contrasting those in more massive stars that require longer for neutrino-driven convection to drive an explosion.
Analysis of the explosion hydrodynamics and direct signals from neutrinos and gravitational waves will enhance our understanding of the CCSN mechanism and its variations, while analysis of the ejecta composition will advance our understanding of chemical evolution.
