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I use high resolution N-body/SPH simulations to model the new proper motionof the Large Magellanic Cloud (LMC) within the Milky Way (MW) halo andinvestigate the effects of gravitational and hydrodynamical forces on theformation of the Magellanic Stream (MS). Both the LMC and the MW are fully selfconsistent galaxy models embedded in extended cuspy LCDM dark matter halos. Ifind that ram-pressure from a low density ionized halo is sufficient to removea large amount of gas from the LMC's disk forming a trailing Stream thatextends more than 120 degrees from the Cloud. Tidal forces elongate thesatellite's disk but do not affect its vertical structure. No stars becomeunbound showing that tidal stripping is almost effectiveless.

Modeling a high velocity LMC. The formation of the Magellanic Stream