  We propose and investigate a new formation mechanism for globular clusters in
which they form within molecular clouds that are formed in the shocked regions
created by galactic winds driven by successive supernova explosions shortly
after the initial burst of massive star formation in the galactic centers. The
globular clusters have a radial distribution that is more extended than that of
the stars because the clusters form as pressure-confined condensations in a
shell that is moving outward radially at high velocity. In addition the model
is consistent with existing observations of other global properties of globular
clusters, as far as comparisons can be made.
