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We present a model for the formation of the Magellanic Stream (MS) due to rampressure stripping. We model the history of the Small and Large MagellanicClouds in the recent cosmological past in a static Milky Way potential withdiffuse halo gas, using observationally motivated orbits for the MagellanicClouds derived from HST proper motions within the potential of the Milky Way.This model is able to reproduce the trailing arm but does not reproduce theleading arm feature, which is common for models of the stream formation thatinclude ram pressure stripping effects. While our model does not outperformother models in terms of matching the observable quantities in the MS, it isclose enough for our ultimate goal -- using the MS to estimate the MW mass.From analyzing our grid of models, we find that there is a direct correlationbetween the observed stream length in our simulations and the mass of the MilkyWay. For the observed MS length, the inferred Milky Way mass is $1.5 \pm 0.32\times 10^{12}$ $M_\odot$, which agrees closely with other independent measuresof the Milky Way mass. We also discuss the MS in the context of HI streams ingalaxy clusters, and find that the MS lies on the low-mass end of a continuumfrom Hickson groups to the Virgo cluster. As a tracer of the dynamical mass inthe outer halo, the MS is a particularly valuable probe of the Milky Way'spotential.

A Dynamical Mass Estimate from the Magellanic Stream