On the initial mass function of population III stars

The collapse and fragmentation of filamentary primordial gas clouds are exp lored using one- and two-dimensional hydrodynamical simulations coupled wit h the nonequilibrium processes of hydrogen molecule formation. The cloud ev olution is computed from the initial central density n(c) = 10-10(6) cm(-3) . The simulations show that depending on the initial density, there are two occasions for the fragmentation of primordial filaments. If a filament has relatively low initial density such as n(c) less than or similar to 10(5) cm(-3), the radial contraction is slow as a result of less effective H-2 co oling and appreciably decelerates at densities higher than a critical densi ty, where LTE populations are achieved for the rotational levels of H-2 mol ecules and the cooling timescale becomes accordingly longer than the free-f all timescale. This filament tends to fragment into dense clumps before the central density reaches 10(8)-10(9) cm(-3), where H-2 cooling by three-bod y reactions is effective and the fragment mass is more massive than some te ns of M.. In contrast, if a filament is initially as dense as n(c) greater than or similar to 10(5) cm(-3), the more effective H-2 cooling with the he lp of three-body reactions allows the filament to contract up to n similar to 10(12) cm(-3). After the density reaches n similar to 10(12) cm(-3), the filament becomes optically thick to H-2 lines and the radial contraction s ubsequently almost stops. At this final hydrostatic stage, the fragment mas s is lowered down to approximate to1 M. because of the high density of the filament. The dependence of the fragment mass upon the initial density coul d be translated into the dependence on the local amplitude of random Gaussi an density fields or the epoch of the collapse of a parent cloud. Hence, it is predicted that the initial mass function of Population III stars is lik ely to be bimodal with peaks of approximate to 10(2) and approximate to1 Mo ., where the relative heights could be a function of the collapse epoch. Im plications for the metal enrichment by Population III stars at high redshif ts and baryonic dark matter are briefly discussed.