Angular momentum distribution during the collapse of primordial
  star-forming clouds
  It is generally believed that angular momentum is distributed during the
gravitational collapse of the primordial star forming cloud. However, so far
there has been little understanding of the exact details of the distribution.
We use the modified version of the Gadget-2 code, a three-dimensional
smoothed-particle hydrodynamics simulation, to follow the evolution of the
collapsing gas in both idealized as well as more realistic minihalos. We find
that, despite the lack of any initial turbulence and magnetic fields in the
clouds the angular momentum profile follows the same characteristic power-law
that has been reported in studies that employed fully self-consistent
cosmological initial conditions. The fit of the power-law appears to be roughly
constant regardless of the initial rotation of the cloud. We conclude that the
specific angular momentum of the self-gravitating rotating gas in the
primordial minihalos maintains a scaling relation with the gas mass as $L
\propto M^{1.125}$. We also discuss the plausible mechanisms for the power-law
distribution.
