  Winds blown from accretion disks formed inside massive rotating stars may
result in stellar explosions observable as Type Ibc and Type II supernovae. A
key feature of the winds is their ability to produce the radioactive Nickel-56
necessary to power a supernova light curve. The wind strength depends on
accretion disk cooling by neutrino emission and photo-disintegration of bound
nuclei. These cooling processes depend on the angular momentum of the stellar
progenitor via the virial temperature at the Kepler radius where the disk
forms. The production of an observable supernova counterpart to a Gamma-Ray
Burst (GRB) may therefore depend on the angular momentum of the stellar
progenitor. Stars with low angular momentum may produce a GRB without making an
observable supernova. Stars with large angular momentum may make extremely
bright and energetic supernovae like SN 1998bw. Stars with an intermediate
range of angular momentum may simultaneously produce a supernova and a GRB.
