On the formation of the Magellanic Stream
نویسندگان
چکیده
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 ionised halo is then sufficient to remove 1.4 × 108M⊙ of gas from the LMC’s disk forming a great circle trailing stream around the Galaxy.
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