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The Magellanic Stream and Leading Arm of HI that stretches from the Large andSmall Magellanic Clouds (LMC and SMC) and over 200 degrees of the Southern skyis thought to be formed from multiple encounters between the LMC and SMC. Inthis scenario, most of the gas in the Stream and Leading Arm is stripped fromthe SMC, yet recent observations have shown a bifurcation of the Trailing Armthat reveals LMC origins for some of the gas. Absorption measurements in theStream also reveal an order of magnitude more gas than in current tidal models.We present hydrodynamical simulations of the multiple encounters between theLMC and SMC at their first pass around the Milky Way, assuming that the Cloudswere more extended and gas rich in the past. Our models create filamentarystructures of gas in the Trailing Stream from both the LMC and SMC. While theSMC trailing filament matches the observed Stream location, the LMC filament isoffset. In addition, the total observed mass of the Stream in these models isunderestimated of a factor of four when the ionized component is accounted for.Our results suggest that there should also be gas stripped from both the LMCand SMC in the Leading Arm, mirroring the bifurcation in the Trailing Stream.This prediction is consistent with recent measurements of spatial variation inchemical abundances in the Leading Arm, which show that gas from multiplesources is present, although the nature is still uncertain.

Models of Tidally Induced Gas Filaments in the Magellanic Stream