I present the results from recent super-computer simulations of early cosmic structure formation. The simulations employ realistic initial conditions that incorporate the baryonic streaming motions, and follow relevant physical processes to the formation of primordial stars. The simulations also follow the post-collapse, accretion-phase evolution of primordial protostars. Fragmentation of circumstellar disks are explained by spiral arm instability. I discuss the characteristic mass of the first stars, multiplicity, and the observational implications. Finally, I present cases that yield super-massive stars with masses greater than 300 Msun. I discuss the origin of massive blackholes in the early universe.

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