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The neutrino-heated "gain layer" immediately behind the stalled shock in a -collapse supernova is unstable to high-Reynolds-number turbulent. We carry out and analyze a new set of 19 high-resolution -dimensional (3D) simulations with a three-species neutrino /heating scheme and compare with spherically-symmetric (1D) and (2D) simulations carried out with the same methods. We study the postbounce supernova evolution in a 15-M_⊙ progenitor star and vary the neutrino heating rate, the magnitude and spatial dependence of from convective burning in the Si/O shell, and spatial resolution. simulations suggest that there is a direct correlation between the strength of turbulence in the gain layer and the susceptability to explosion. 2D and 3D simulations explode at much lower neutrino heating rates than 1D simulations. is commonly explained by the fact that nonradial dynamics allows accreting to stay longer in the gain layer. We show that this explanation is. Our results indicate that the effective turbulent ram pressure on the shock plays a crucial role by allowing multi-D models to explode a lower postshock thermal pressure and thus with less neutrino heating than 1D models. We connect the turbulent ram pressure with turbulent energy at large and in this way explain why 2D simulations are erroneously exploding easily than 3D simulations.
Couch et al. (Fri,) studied this question.