On the formation of the Magellanic Stream

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dc.creatorMastropietro, C.
dc.creatorMoore, B.
dc.creatorMayer, L.
dc.creatorStadel, J.
dc.creatorWadsley, J.
dc.date2003-09-09
dc.date.accessioned2026-07-07T02:09:29Z
dc.date.available2026-07-07T02:09:29Z
dc.descriptionWe 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.
dc.description4 pages, 2 figures, to be published in the proceedings of the "Satellite and Tidal Streams", La Palma 26-30 May 2003, Spain, eds. F. Prada, D. Martinez-Delgado, T. Mahoney
dc.identifierhttps://arxiv.org/abs/astro-ph/0309244
dc.identifierhttp://arxiv.org/abs/astro-ph/0309244
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/6450
dc.subjectAstrophysics
dc.titleOn the formation of the Magellanic Stream
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