Numerical Simulations of the Magellanic System - Part One - Orbits of the Magellanic Clouds and the Global Gas Distribution

Details Numerical Simulations of the Magellanic System - Part One - Orbits of the Magellanic Clouds and the Global Gas Distribution Numerical Simulations of the Magellanic System - Part One - Orbits of the Magellanic Clouds and the Global Gas Distribution

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994mnras.266..567g&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 266, NO. 3/FEB1, P. 567, 1994

Astronomy and Astrophysics

Astronomy

132

Scientific paper

The numerical model of the Galaxy and the Large and Small Magellanic Clouds devised by Mural & Fujimoto is employed, with revised values of various observational parameters, to reproduce the global gas distribution in the Magellanic system by a test-particle simulation. The Magellanic orbits that achieve the best reproduction of the Magellanic Stream and the inter-Cloud Bridge place the LMC and the SMC in a binary state for the past 15 Gyr, with a close encounter between the Magellanic Clouds occurring 0.2 Gyr ago at a minimum separation of 7 kpc. By performing a test-particle simulation with 20000 particles representing the LMC and SMC discs, a detailed comparison can be made with observations of the structure of the Magellanic Clouds and inter-Cloud Bridge. In particular, the large extent in depth of the SMC, shell-like irregularities in the outer part of the LMC, and distinct gas masses in the inter-Cloud Bridge region are shown to result from the tidal interactions of the Magellanic system. The Magellanic Stream is modelled as a product of the tidal interaction of the Magellanic Clouds with the Galaxy, and some criticisms of the standard tidal model for the origin of the Magellanic Stream are addressed.

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