Abstract:
By combining Fornax, FLASH, and Sedona, we have built a pipeline that can evolve a massive star from core collapse to shock breakout (or black hole formation) in full 3D. Compared to the widely used spherical (1D) models, the explosion asymmetry that naturally emerges in 3D simulations can significantly modify the CCSN outcomes. In this talk, I will present some new insights extracted from these long-term 3D CCSN simulations, including the asymmetric shock breakout, the distribution and mixing of elements, and the black hole formation channels. I will also mention the challenges in future simulations, such as the effects of neutrino oscillations and the formation of potential central engines。
