Common envelope evolution spins up the core of a massive star before it explodes. I show the decisive effects of a high rotation rate on the dynamics of core-collapse supernovae using detailed three-dimensional simulations including core deleptonization and approximate neutrino transport. The simulations indicate that the collapse of rapidly-rotating massive stellar cores leads to super-energetic supernovae with strong asymmetry. Due to non-spherical mass ejection during the common envelope evolution phase, the scenario I present establishes a strong connection between super-energetic supernovae and their interaction with a bipolar massive circumstellar medium.