Numerical simulations of the Magellanic system – I. Orbits of the Magellanic Clouds and the global gas distribution

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Abstract
The numerical model of the Galaxy and the Large and Small Magellanic Clouds devised by Murai & 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 20 000 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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