Paper:	N-body Simulations of the Magellanic Stream
Volume:	166, Stromlo Workshop on High-Velocity Clouds
Page:	292
Authors:	Gardiner, Lance T.
Abstract:	N-body simulations have been successfully employed to model the Magellanic Stream as a tidal tail torn from the Magellanic Clouds by the Galaxy. The asymmetry introduced by the LMC-SMC binary interaction leads to a long tidal tail with a weaker leading arm. The inclusion of gas-dynamical effects and star formation has added further refinements to this picture and provides a possible explanation for the apparent absence of stars in the Magellanic Stream. New work on simulations involving a more realistic LMC disk-type potential and a weak drag force due to diffuse gas in the Galactic halo is also presented.

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