Total angular momentum and rotational velocity of the runaway at around 1000 s after the explosion. The plotted quantities are spherical averages and highlight the differences in the state of the stellar interior. Most of the angular momentum is within 0.1 R_⊙. While the external (> 0.1 R_⊙) has some residual rotation and radial energy this is only in a small region that forms a stream-like structure.