Using a new physical model for star formation ( Padoan 1995 ) we have tested the possibility that globular clusters ( GCs ) are formed from primordial mass fluctuations , whose mass scale ( 10 ^ { 8 } - 10 ^ { 9 } M _ { \odot } ) is selected out of a CDM spectrum by the mechanism of non-equilibrium formation of H _ { 2 } .

We show that such clouds are able to convert about 0.003 of their total mass into a bound system ( GC ) and about 0.02 into halo stars .
The metal enriched gas is dispersed 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 which is a consequence of the universal statistics of fluid turbulence .
They also depend on the ratio of baryonic over non-baryonic mass , X _ { b } , and are comparable with the values observed in typical spiral galaxies for X _ { b } \approx 0.1 - 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 .

The model 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 in primordial clouds leads to a large number of supernovae and to a high blue luminosity during the first two Gyr of the life of every galaxy .