Ram Pressure Processes in the Galactic Halo and Formation of the Magellanic Stream

Details Ram Pressure Processes in the Galactic Halo and Formation of the Magellanic Stream Ram Pressure Processes in the Galactic Halo and Formation of the Magellanic Stream

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..331...89m&link_type=abstract

Extra-Planar Gas, ASP Conference Proceedings, Vol. 331. Edited by Robert Braun. Proceedings of the meeting held at Dwingeloo,

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We use 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 and gaseous disks of the two galaxies. Tidal forces distort the LMC's disk, forcing a bar and creating a very strong warp and a diffuse stellar halo, although very few stars are unbound from the LMC. Ram pressure from a low density ionized Galactic halo is then sufficient to remove 1.3 × 108 M&sun; of gas from the LMC's disk forming a great circle trailing stream around the Galaxy.

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