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Models for the dynamical evolution of the Magellanic System

Published online by Cambridge University Press:  01 July 2008

Kenji Bekki
Kenji Bekki*
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW, 2052, Australia email: bekki@phys.unsw.edu.au
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Abstract

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I discuss the following five selected topics on formation and evolution of the LMC and the SMC based on fully self-consistent chemodynamical simulations of the Magellanic Clouds (MCs): (1) formation of bifurcated gaseous structures and young stars in the Magellanic bridge (MB), (2) formation of the Magellanic stream (MS) due to the tidal interaction between the LMC, the SMC, and the Galaxy within the last 2 Gyrs, (3) origin of the observed kinematical differences between H i gas and stars in the SMC, (4) formation of stellar structures dependent on their ages and metallicities in the LMC, and (5) a new common halo model explaining both the latest HST ACS observations on the proper motions of the LMC and the SMC and the presence of the MS in the Galactic halo. I focus exclusively on the latest developments in numerical simulations on formation and evolution of the Magellanic system.

Keywords

galaxies: evolutiongalaxies: halosgalaxies: interactionsgalaxies: kinematics and dynamicsMagellanic Cloudsgalaxies: stellar contentdark matter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S256: The Magellanic System: Stars, Gas, and Galaxies , July 2008 , pp. 105 - 116
Copyright
Copyright © International Astronomical Union 2009

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