Core collapse of rotating massive stars

Massive stars are known to be rotating while on the main sequence, though it is difficult to extrapolate their angular momentum distribution upon reaching core collapse at the end of their lives, which is affected by binary interactions and internal transport processes. While numerous simulations of core collapse focus on specific non-rotating progenitor models, relatively little attention is given to the collapse of rapidly rotating stars. I will present numerical simulations of core collapse in rotating stars, with different rotation rates, and discuss the different dynamics and implications for supernova explosions.