  Recent observations have revealed that velocity dispersions of
``ultra-compact dwarf'' (UCD) galaxies are significantly smaller than those of
other galaxy populations in the Fornax and the Virgo clusters of galaxies. In
order to understand the origin of the observed lower velocity dispersions of
UCDs, we numerically investigate line-of-sight velocity dispersion (sigma_los)
of galaxy populations with variously different orbits in clusters of galaxies
with the total masses of M_cl. We particularly investigate radial velocity
dispersion profiles (sigma_los(R)) and velocity dispersions within the central
200 kpc of a cluster model (sigma_m) for galaxies with different pericenter
distances (r_p) and orbital eccentricities (e) in the model with M_cl = 7.0 x
10^13 M_sun reasonable for the Fornax cluster. We find that sigma_los(R) and
sigma_m of galaxies with smaller r_p are steeper and smaller, respectively, for
a given initial e distribution of galaxies. For example, we find that sigma_m
is ~ 260 km/s for galaxies with r_p <50 kpc and ~ 336 km/s for all galaxies in
the model with the mean e of 0.6. These results imply that the observed lower
velocity dispersion of UCD population is consistent with the UCDs having
significantly smaller r_p than other galaxy populations in the Fornax. We
discuss these results in the context of the ``galaxy threshing'' scenario in
which UCDs originate from nuclei of nucleated dwarf galaxies. We suggest that
the observed differences in kinematical properties between UCDs and other dwarf
galaxy populations in clusters of galaxies can be understood in terms of the
differences in orbital properties between UCDs and the dwarf populations.
