On star formation in primordial protoglobular clouds

Using a new physical model for star formation (Padoan 1995) we have testedthe possibility that globular clusters (GCs) are formed from primordial massfluctuations, whose mass scale ($10^8$ - $10^9$ M$_{\odot}$) is selected out ofa CDM spectrum by the mechanism of non-equilibrium formation of $H_2$. We showthat such clouds are able to convert about 0.003 of their total mass into abound system (GC) and about 0.02 into halo stars. The metal enriched gas isdispersed away from the GC by supernova explosions and forms the galactic disk.These mass ratios between GCs, halo and disk depend on the predicted IMF whichis a consequence of the universal statistics of fluid turbulence. They alsodepend on the ratio of baryonic over non-baryonic mass ,$X_b$, and arecomparable with the values observed in typical spiral galaxies for $X_b \approx0.1-0.2$. The computed mass and radius for a GC ( $5\times 10^5$ M$_{\odot}$and 30 pc) are in good agreement with the average values in the Galaxy. Themodel predicts an exponential cut off in the stellar IMF below 0.1 M$_{\odot}$in GCs and 0.6 M$_{\odot}$ in the halo. The quite massive star formation inprimordial clouds leads to a large number of supernovae and to a high blueluminosity during the first two Gyr of the life of every galaxy