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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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