On the effects of rotation during the formation of population III
  protostars
  It has been suggested that turbulent motions are responsible for the
transport of angular momentum during the formation of Population III stars,
however the exact details of this process have never been studied. We report
the results from three dimensional SPH simulations of a rotating
self-gravitating primordial molecular cloud, in which the initial velocity of
solid-body rotation has been changed. We also examine the build-up of the discs
that form in these idealized calculations.
