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In this paper, we present the results of our three-dimensional, multi-group,multi-neutrino-species radiation/hydrodynamic simulation using thestate-of-the-art code F{\sc{ornax}} of the terminal dynamics of the core of anon-rotating 16-M$_{\odot}$ stellar progenitor. The calculation incorporatesredistribution by inelastic scattering, a correction for the effect ofmany-body interactions on the neutrino-nucleon scattering rates, approximategeneral relativity (including the effects of gravitational redshifts),velocity-dependent frequency advection, and an implementation of initialperturbations in the progenitor core. The model explodes within $\sim$100milliseconds of bounce (near when the silicon-oxygen interface is accretedthrough the temporarily-stalled shock) and by the end of the simulation (here,$\sim$677 milliseconds after bounce) is accumulating explosion energy at a rateof $\sim$2.5$\times$10$^{50}$ ergs s$^{-1}$. The supernova explosion resemblesan asymmetrical multi-plume structure, with one hemisphere predominating. Thegravitational mass of the residual proto-neutron star at $\sim$677 millisecondsis $\sim$1.42 M$_{\odot}$. Even at the end of the simulation, explosion in mostof the solid angle is accompanied by some accretion in an annular fraction atthe wasp-like waist of the debris field. The ejecta electron fraction (Y$_e$)is distributed from $\sim$0.48 to $\sim$0.56, with most of the ejecta massproton-rich. This may have implications for supernova nucleosynthesis, andcould have a bearing on the p- and $\nu$p-processes and on the site of thefirst peak of the r-process. The ejecta spatial distributions of both Y$_e$ andmass density are predominantly in wide-angle plumes and large-scale structures,but are nevertheless quite patchy.

A Successful 3D Core-Collapse Supernova Explosion Model