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On the formation of the Magellanic Stream

C. Mastropietro·B. Moore·L. Mayer·J. Stadel·J. Wadsley
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Abstract

We use high resolution N-Body/SPH simulations to study the hydro-dynamical 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 $1.4 \times 10^8M_\odot$ of gas from the LMC's disk forming a great circle trailing stream around the Galaxy.

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C. Mastropietro, B. Moore, L. Mayer, J. Stadel, J. Wadsley. 2003-09-09. On the formation of the Magellanic Stream. https://arxiv.org/abs/astro-ph/0309244

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