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N-body simulations of the small Magellanic Cloud and the magellanic stream
Gardiner, L.T.,Nogouchi, M. 선문대학교 1994 鮮文論叢 自然科學 編 Vol.- No.4
An extensive set of N-body simulations has been carried out on the gravitational interaction of the Small Magellanic Cloud (SMC) with the Galaxy and the Large Magellanic Cloud (LMC), The SMC is assumed to have been a barred galaxy with a disc-to-halo mass ratio of unity before interaction and modelled by a large number of self-gravitating particles, whereas the Galaxy and LMC have been represented by rigid spherical potentials. Our more advanced numerical treatment has enabled us to obtain the most integrated and systematic understanding to date of numerous morphological and kinematical features observed in t,heMagellanic system (exclucling the LMC), which have been dealt with more or less separately in previous studies. The best model we have found succeeded in reproducing the Magellanic Stream (MS) as a tidal plume created by the SMC-LMC-Galaxy close encounter 1.5 Gyr ago. At the same time, we see the formation of a leading counterpart to the Magellanic Stream (the leading arm), on the opposite side of the Magellanic Clouds to the Stream, which mimicks the overall distribution of several neutral hydrogen clumps observed in the corresponding region of the sky. A close encounter with the LMC 0.2 Gyr ago created another tidal tail and bridge system, which constitutes the inter-Cloud region in our model. The elongation of the SMC bar along the line-of-sight direction suggested by Cepheid observations has been partially reproduced, alongside its projected appearance on the sky. The model successfully explains some major trends in the kinematics of young populations in the SMC bar and older populations in the 'halo' of the SMC, as well as the overall velocity pattern for the gas, young stars, and carbon stars in the inter-Cloud region.
Gardiner, L.T.,Sawa, T.,Fujimoto, M. 성화대학교 1993 成和論叢 Vol.- No.3
The numerical model of the Galaxy, Large and Small Magellanic Clouds devised by Murai & Fujimoto(1980) has been 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 which achieved 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 detailed comparison could 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 were 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.
SIMULATIONS OF THE INTERACTING MAGELLANIC SYSTEM
GARDINER LANCE T.,NOGUCHI MASAFUMI The Korean Astronomical Society 1996 Journal of The Korean Astronomical Society Vol.29 No.suppl1
The Galaxy and the Large and Small Magellanic Clouds (LMC and SMC respectively) form a triple system of mutually interacting galaxies. We have carried out a set of N-body simulations on the gravitational interaction of the SMC with the Galaxy and the LMC in order to model prominent features such as the Magellanic Stream, the inter-Cloud Bridge, and the large depth of the SMC which are thought to be products of the tidal interactions among the members of this system.