  We investigate the formation of a number of key large-scale HI features in
the ISM of the Magellanic Bridge using dissipationless numerical simulation
techniques. This study comprises the first direct comparison between detailed
HI maps of the Bridge and numerical simulations. We confirm that the SMC forms
two tidal filaments: a near arm, which forms the connection between the SMC and
LMC, and a counterarm. We show that the HI of the most dense part of the Bridge
can become arranged into a bimodal configuration, and that the formation of a
"loop" of HI, located off the North-Eastern edge of the SMC can be reproduced
simply as a projection of the counter-arm, and without invoking localised
energy-deposition processes such as SNe or stellar winds.
