  We present the first complete 3-dimensional simulations of the core-collapse
of a massive star from the onset of collapse to the resultant supernova
explosion. We compare the structure of the convective instabilities that occur
in 3-dimensional models with those of past 2-dimensional simulations. Although
the convective instabilities are clearly 3-dimensional in nature, we find that
both the size-scale of the flows and the net enhancement to neutrino heating
does not differ greatly between 2- and 3-dimensional models. The explosion
energy, explosion timescale, and remnant mass does not differ by more than 10%
between 2- and 3-dimensional simulations.
