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The Magellanic Clouds have lost most of their gas during their passage by theMilky Way, a property that has never been successfully modeled. Here we useaccurate and mesh-free hydrodynamic simulations to reproduce the MagellanicStream and the Magellanic Clouds in the frame of a 'ram-pressure pluscollision' model. This model reproduces many of the observed properties of theHI Stream including most of its density profile along its length and its dualfilamentary structure. Besides this, ram-pressure combined withKelvin-Helmholtz instabilities extracts amounts of ionized and HI gasconsistent with those observed. The modeled scenario also reproduces theMagellanic Bridge, including the offset between young and old stars, and thecollision between the Clouds, which is responsible of the very elongatedmorphology of the Small Magellanic Cloud along the line of sight. This modelhas solved most of the mysteries linked to the formation of the MagellanicStream. The Leading Arm is not reproduced in the current model because itrequires an alternative origin.

Toward a Complete Understanding of the Magellanic Stream Formation