  We present the results of 3-dimensional simulations of the direct collapse to
a black hole of a rotating, 60-solar-mass, zero metallicity, population III
star. Because the structure of this star (angular momentum, density and
temperature profiles) is similar to many collapsar gamma-ray burst progenitors,
these calculations have implications beyond the fate of population III stars.
These simulations provide a first 3-dimensional look at a realistic collapsar
progenitor, and the results are very different from any previous 2-dimensional
calculations. If the angular momentum of the progenitor is high,
non-axisymmetric instabilities in the collapsing core cause spiral structures
to form, and these structures shape later outflows. These outflows are driven
by the imbalance between viscous heating and inefficient neutrino cooling and
ultimately develop into a 1e52 erg explosion. Without magnetic fields, this
collapse will not produce relativistic jets, but the explosion is indeed a
hypernova. We conclude with a discussion of the implications of such
calculations on the explosions, nucleosynthesis, neutrino flux and
gravitational wave emission from the collapse of massive stars.
