  The origin of metal-rich, highly flattened, and rapidly rotating disk
globular cluster system in the Galaxy is one of longstanding issues in the
context of the Galaxy formation. Our numerical simulations suggest a new
``two-fold'' scenario that the disk globular clusters are firstly formed in the
high-pressure, dense central region of a gas-rich dwarf galaxy, as induced
during the tidal interaction with the pre-existing, young thin disk of the
Galaxy, and then dispersed into the disk region owing to the final tidal
destruction of the merging dwarf. We also demonstrate that spatial
distribution, total number, and metallicity distribution of the clusters formed
in this minor merging depend on the mass ratio of the host to dwarf galaxy and
the orbital configuration of merging. Based on these results, we discuss
whether a minor merging event about 10 Gyr ago can explain both the Galactic
thick disk and the disk globular clusters. Several other implications for the
possible relation between the properties of disk galaxies and their disk
globular clusters are also discussed.
