Were the Old Halo globular clusters able to sustain a self-enrichment phase?

It has been argued for a long time that the self-enrichment process could not occur within proto-globular clouds because of the supernova energetics. We revisit this argument and demonstrate that it may not be true. Since not all the kinetic energy of Type II Supernovae is deposited as kinetic energy of the ISM, we suggest comparing the binding energy of the progenitor cloud to the kinetic energy of the ISM instead of the kinetic energy of the Type II Supernova ejecta. This criterion is used to study the disruptive ability of Type II Supernovae onto proto-globular clouds. It is found that the early chemical history of globular clusters is greatly influenced by the pressure exerted by the external medium on their progenitor clouds.