Core-Collapse Supernovae are triggered in their interiors by the collapse of the inert iron cores formed at the end-stage of stellar evolution for massive stars. The shock wave that eventually unbinds most of the presupernova star is formed when the collapsing matter reaches nuclear densities and the protoneutron star forms. In the current theory, the implosion is successfully turned into an explosion that is energized to canonical values of ~0.5-1 Bethe by neutrino heating in the layers just above the protoneutron star.  This is necessarily aided by multidimensional matter motions like convection and turbulence in the  heating layers formed at the onset of the explosion and also likely in the presupernova progenitor structure itself. In this talk, I will review the current state of core-collapse supernova simulations, present results of recent 3D simulations using the FLASH hydrodynamics code, and discuss a recent global comparison between many core-collapse supernovae groups.