NDLI: Evolution of the Small Magellanic Cloud

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Evolution of the Small Magellanic Cloud

Content Provider	Semantic Scholar
Author	Bekki, Kenji
Copyright Year	2008
Abstract	We investigate (1) the origin of the bifurcation of the Magellanic stream (MS), (2) the formation of distinctively metal-poor stellar populations in the Large Magellanic Cloud (LMC) due to sporadic gas transfer from the SMC, and (3) the collision between the leading arms (LAs) of the MS and the outer part of the Galactic HI disk based on numerical simulations of LMC-SMCGalaxy interaction for the last 2.5 Gyr (e.g., Bekki & Chiba 2007, BC07). We adopt numerical methods and techniques of the simulations on the evolution of the MCs used in our previous papers (Bekki & Chiba 2005; B05): we first determine the most plausible and realistic orbits of the MCs by using “ the backward integration scheme” (for orbital evolution of the MCs) by Murai & Fujimoto (1980) for the last 2.5 Gyr and then investigate the evolution of the MCs using GRAPE systems (Sugimoto et al.1990). The total masses of the LMC and the SMC are set to be 2.0×10M⊙ and 3.0×10 M⊙, respectively, in all models. The SMC is represented by a fully self-consistent dynamical model wheres the LMC is represented by a point mass. We adopt the initial locations and velocities of the MCs with respect to the Galaxy that are similar to those adopted by BC07.
File Format	PDF HTM / HTML
Alternate Webpage(s)	http://arxiv.org/pdf/0707.4566v1.pdf
Language	English
Access Restriction	Open
Subject Keyword	Alveolar rhabdomyosarcoma Bifurcation theory Biological Evolution Clique problem Coat of arms Dynamical system Entity Name Part Qualifier - adopted GRAPE Little man computer Lymphoma, Large-Cell, Follicular Magellanic Catalogue of Stars Molecular orbital Numerical method Ocular orbit Paper Population Simulation Stellar (payment network) organelle membrane contact site subrhabdomeral cisterna
Content Type	Text
Resource Type	Article

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