  We present a high-resolution simulation of globular cluster formation in a
galaxy merger. For the first time in such a simulation, individual star
clusters are directly identified and followed on their orbits. We
quantitatively compare star formation in the merger to that in the unperturbed
galaxies. The merging galaxies show a strong starburst, in sharp contrast to
their isolated progenitors. Most star clusters form in the tidal features. With
a mass range of $5\times10^{5}$--$5\times 10^{6} M_{\odot}$, they are
identified as globular clusters. The merger remnant is an elliptical galaxy.
Clusters with different mass or age have different radial distributions in the
galaxy. Our results show that the high specific frequency and bimodal
distribution of metallicity observed in elliptical galaxies are natural
products of gas-rich mergers, supporting a merger origin for the ellipticals
and their globular cluster systems.
