We use very high-resolution simulations of galaxy-galaxy collisions to
study the formation of globular clusters. Our simulations resolve the
multiphase nature of the inter-stellar medium, and thus can be used to
locate star-forming sites robustly. We use a total of 1.5 X 10^7
particles to represent two gas-rich progenitor galaxies. During the
first encounter, a very large filament is formed at the collision
interface of the colliding galaxies. The filament's mass is ~ 10^9 Msun, and it consists mostly of dense and cold gases. The peak star
formation rate in the filament reaches ~ 15 Msun yr^-1. Eleven
self-bound star clusters are located in the giant filament after the starburst.
These star clusters have masses of ~ 10^(6-7) Msun. They have little
dark matter content. Star formation in individual star clusters is
quenched in about ~ 10^7 yr; feedback effects of Type II
supernovae are significant in the small mass systems. Consequently,
stars in a cluster have a nearly uniform metallicity composition. The
formation efficiency of star clusters in the filament, Mstars/Mfilament, is found to be ~ 0.18. at the final stage
of the star cluster formation. Star clusters formed in this manner have
simialr characteristic to observed metal-rich globular clusters.