cores of many massive-star models in three spatial dimensions. This is the
most comprehensive set of realistic 3D core-collapse supernova (CCSN)
simulations yet performed and has provided very important insights into
the mechanism and character of this 60-year-old astrophysical puzzle. Most
3D models explode naturally and without artifice by the neutrino
mechanism, aided by turbulent convection. I will present detailed results
from this suite of runs and the novel conclusions derived from our new
capacity to simulate many 3D, as opposed to 2D and 1D, full physics models
every year. Emerging are insights into the criteria for explosion, the
systematics of explosion energy and residual neutron-star mass with
progenitor, the characteristics of proto-neutron star convection, neutrino
and gravitational-wave emissions and signatures, the morphology of CCSN
explosions, and supernova nucleosynthesis. This new capability, enabled
by this new algorithm and modern HPC assets, is poised to transform our
understanding of this central astrophysical phenomenon.