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We use the moving-mesh code AREPO to investigate the effects of differentlevels of rotation and turbulence on the fragmentation of primordial gas andthe formation of Population III stars. We consider 9 different combinations ofturbulence and rotation and carry out 5 different realizations of each setup,yielding one of the largest sets of simulations of Population III starformation ever performed. We find that fragmentation in Population IIIstar-forming systems is a highly chaotic process and show that the outcomes ofindividual realizations of the same initial conditions often varysignificantly. However, some general trends are apparent. Increasing theturbulent energy promotes fragmentation, while increasing the rotational energyinhibits fragmentation. Within the 1000 yr period that we simulate, runsincluding turbulence yield flat protostellar mass functions while purelyrotational runs show a more top-heavy distribution. The masses of theindividual protostars are distributed over a wide range from a few $10^{-3} \,{\rm M_{\odot}}$ to several tens of ${\rm M_\odot}$. The total mass growth rateof the stellar systems remains high throughout the simulations and depends onlyweakly on the degree of rotation and turbulence. Mergers between protostars arecommon, but predictions of the merger fraction are highly sensitive to thecriterion used to decide whether two protostars should merge. Previous studiesof Population III star formation have often considered only one realization perset of initial conditions. However, our results demonstrate that robust trendscan only be reliably identified by considering averages over a larger sample ofruns.

monthly notices of the royal astronomical society

Formation sites of Population III star formation: The effects of  different levels of rotation and turbulence on the fragmentation behavior of  primordial gas