  Multi-dimensional instabilities have become an important ingredient in
core-collapse supernova (CCSN) theory. Therefore, it is necessary to understand
the driving mechanism of the dominant instability. We compare our parameterized
three-dimensional CCSN simulations with other buoyancy-driven simulations and
propose scaling relations for neutrino-driven convection. Through these
comparisons, we infer that buoyancy-driven convection dominates post-shock
turbulence in our simulations. In support of this inference, we present four
major results. First, the convective fluxes and kinetic energies in the
neutrino-heated region are consistent with expectations of buoyancy-driven
convection. Second, the convective flux is positive where buoyancy actively
drives convection, and the radial and tangential components of the kinetic
energy are in rough equipartition (i.e. K_r ~ K_{\theta} + K_{\phi}). Both
results are natural consequences of buoyancy-driven convection, and are
commonly observed in simulations of convection. Third, buoyant driving is
balanced by turbulent dissipation. Fourth, the convective luminosity and
turbulent dissipation scale with the driving neutrino power. In all, these four
results suggest that in neutrino-driven explosions, the multi-dimensional
motions are consistent with neutrino-driven convection.
