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Paper: On the Formation of the Magellanic Stream
Volume: 327, Satellites and Tidal Streams
Page: 234
Authors: Mastropietro, C.; Moore, B.; Mayer, L.; Stadel, J.; Wadsley, J.
Abstract: We use high resolution N-body/SPH simulations to study the hydrodynamical and gravitational interaction between the Large Magellanic Cloud and the Milky Way. We model the dark and hot extended halo components, as well as the stellar/gaseous disks of the two galaxies. Tidal forces distort the LMC's disk, forcing a bar and creating a diffuse stellar halo and a strong warp, although very few stars are unbound from the LMC. Ram pressure from a low density ionized halo is then sufficient to remove 1.4 x 108 MSolar of gas from the LMC's disk forming a great circle trailing stream around the Galaxy.
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