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We perform a large set of cosmological simulations of early structureformation and follow the formation and evolution of 1540 star-forming gasclouds to derive the mass distribution of primordial stars. The star formationin our cosmological simulations is characterized by two distinct populations,the so-called Population III.1 stars and primordial stars formed under theinfluence of far ultraviolet (FUV) radiation (Population III.2D stars). In thiswork, we determine the stellar masses by using the dependences on the physicalproperties of star-forming cloud and/or the external photodissociatingintensity from nearby primordial stars, which are derived from the results oftwo-dimensional radiation hydrodynamic simulations of protostellar feedback.The characteristic mass of the Pop III stars is found to be a few hundred solarmasses at z ~ 25, and it gradually shifts to lower masses with decreasingredshift. At high redshifts z > 20, about half of the star-forming gas cloudsare exposed to intense FUV radiation and thus give birth to massive Pop III.2Dstars. However, the local FUV radiation by nearby Pop III stars becomes weakerat lower redshifts, when typical Pop III stars have smaller masses and the meanphysical separation between the stars becomes large owing to cosmic expansion.Therefore, at z < 20, a large fraction of the primordial gas clouds host PopIII.1 stars. At z =< 15, the Pop III.1 stars are formed in relatively cool gasclouds due to efficient radiative cooling by H_2 and HD molecules; such starshave masses of a few x 10 Msun. Since the stellar evolution and the final fateare determined by the stellar mass, Pop III stars formed at different epochsplay different roles in the early universe.

Primordial Star Formation under the Influence of Far Ultraviolet Radiation: 1540 Cosmological Halos and the Stellar Mass Distribution