  An important result in core-collapse supernova (CCSN) theory is that
spherically-symmetric, one-dimensional simulations routinely fail to explode,
yet multi-dimensional simulations often explode. Numerical investigations
suggest that turbulence eases the condition for explosion, but how is not fully
understood. We develop a turbulence model for neutrino-driven convection, and
show that this turbulence model reduces the condition for explosions by about
30%, in concordance with multi-dimensional simulations. In addition, we
identify which turbulent terms enable explosions. Contrary to prior
suggestions, turbulent ram pressure is not the dominant factor in reducing the
condition for explosion. Instead, there are many contributing factors, ram
pressure being only one of them, but the dominant factor is turbulent
dissipation (TD). Primarily, TD provides extra heating, adding significant
thermal pressure, and reducing the condition for explosion. The source of this
TD power is turbulent kinetic energy, which ultimately derives its energy from
the higher potential of an unstable convective profile. Investigating a
turbulence model in conjunction with an explosion condition enables insight
that is difficult to glean from merely analyzing complex multi-dimensional
simulations. An explosion condition presents a clear diagnostic to explain why
stars explode, and the turbulence model allows us to explore how turbulence
enables explosion. Though we find that turbulent dissipation is a significant
contributor to successful supernova explosions, it is important to note that
this work is to some extent qualitative. Therefore, we suggest ways to further
verify and validate our predictions with multi-dimensional simulations.
