  Our numerical simulations first demonstrate that the pressure of ISM in a
major merger becomes so high ($>$ $10^5$ $\rm k_{\rm B}$ K $\rm cm^{-3}$) that
GMCs in the merger can collapse to form globular clusters (GCs) within a few
Myr. The star formation efficiency within a GMC in galaxy mergers can rise up
from a few percent to $\sim$ 80 percent, depending on the shapes and the
temperature of the GMC. This implosive GC formation due to external high
pressure of warm/hot ISM can be more efficient in the tidal tails or the
central regions of mergers. The developed clusters have King-like profile with
the effective radius of a few pc. The structural, kinematical, and chemical
properties of these GC systems can depend on orbital and chemical properties of
major mergers.
