  An extensive set of N-body simulations has been carried out on the
gravitational interaction of the Small Magellanic Cloud (SMC) with the Galaxy
and the Large Magellanic Cloud (LMC). The SMC is assumed to have been a barred
galaxy with a disc-to-halo mass ratio of unity before interaction and modelled
by a large number of self-gravitating particles, whereas the Galaxy and LMC
have been represented by rigid spherical potentials. The best model we have
found succeeded in reproducing the Magellanic Stream (MS), as well as a leading
counterpart to the Magellanic Stream (the leading arm), on the opposite side of
the Magellanic Clouds to the Stream, which mimicks the overall distribution of
several neutral hydrogen clumps observed in the corresponding region of the
sky. The elongation of the SMC bar along the line-of-sight direction suggested
by Cepheid observations has been partially reproduced, alongside its projected
appearance on the sky. The model successfully explains some major trends in the
kinematics of young populations in the SMC bar and older populations in the
`halo' of the SMC, as well as the overall velocity pattern for the gas, young
stars, and carbon stars in the inter-Cloud region.
