  Recent observations on structural properties of the Large Magellanic Cloud
(LMC) based on the Deep Near-Infrared Southern Sky Survey (DENIS) and Two
Micron All-Sky Survey (2MASS) have revealed that the LMC has an off-center bar
even in the older stellar populations. Previous dynamical models including
tidal interaction between the LMC, the Small Magellanic Cloud (SMC), and the
Galaxy, however, did not reproduce so well the older off-center bar. We here
show that the off-center bar can be formed if the LMC with an already existing
bar can collide with a low-mass Galactic subhalo as massive as 5 * 10^8 M_sun
(corresponding roughly to a few % of the LMC mass). The simulated stellar
distribution after the collision appears to show an ``off-center bar'', not
because the center of the bar significantly deviates from the dynamical center
of the LMC, but because the underlying stellar distribution of the disk is
significantly asymmetric with respect to the center of the bar. We discuss
whether off-center bars observed in Magellanic-type dwarf galaxies can be
formed as a result of tidal interaction with low-mass halos with no or little
visible matters.
