What prerequisite condition, revealed by three-dimensional simulations, is necessary to help the shock wave survive and revive?

Pre-existing turbulence generated during the final silicon burning phase

Early, simpler models suggested the shock wave would easily blow the star apart, but detailed simulations showed the initial shock stalls quickly due to energy loss processes like re-initiating photodisintegration. The key ingredient identified for the shock wave to overcome this stalling and successfully revive is rooted in complex fluid dynamics. Specifically, three-dimensional models highlight powerful, turbulent convection occurring in the layers just preceding the collapse, driven during the final silicon burning phase. This inherent turbulence and the resulting asymmetric structure are considered crucial for imparting the necessary boost or complexity needed for the shock to be reignited, rather than relying on simplistic symmetric models.