scholarly journals The interacting Magellanic System

1991 ◽  
Vol 148 ◽  
pp. 447-452 ◽  
Author(s):  
S. R. Wayte
Keyword(s):  
Magellanic Clouds ◽  
Entire Length ◽  
Tidal Model ◽  
The Past ◽  
Multi Phase ◽  
Magellanic Stream ◽  
Insight Into ◽  
Magellanic System ◽  
Anomalous Velocity

The Magellanic System is viewed focusing on the global interactions in the System. These give insight into its history and structure. The past orbits of the Magellanic Clouds (MCs) are examined. A tidal encounter between the Large and Small Magellanic Clouds (LMC, SMC) has almost certainly occurred within the last 109 yrs. This hypothesis is supported by the observed structure of the Magellanic System, and so is accepted. The Magellanic Stream is an indirect result of the tidal encounter which is crucial to understanding the Magellanic System. It is a complex interacting gas feature, bifurcated along its entire length with many anomalous velocity H I clouds alongside. The possible models for the Magellanic Stream are examined and here I propose that its origin is due to the collision of a multi-phase halo with the vast region of gas between the LMC and the SMC. In this respect the polar subsystem around our Galaxy is seen to be particularly important. The popular tidal model for the origin of the Magellanic Stream fails to satisfy key observational features, and is thus rejected.

scholarly journals The Kinematics of the Magellanic Clouds

1995 ◽  
Vol 166 ◽  
pp. 273-282
Author(s):  
B.E. Westerlund
Keyword(s):  
Galactic Halo ◽  
Neutral Hydrogen ◽  
Magellanic Clouds ◽  
Great Promise ◽  
Common Envelope ◽  
The Past ◽  
Ram Pressure ◽  
Long Time ◽  
Magellanic Stream ◽  
Magellanic System

It is essential for our understanding of the evolution of the Magellanic System, comprising the Large and the Small Magellanic Cloud, the Intercloud or Bridge region and the Magellanic Stream, to know its motions in the past. The Clouds have a common envelope of neutral hydrogen; this indicates that they have been bound to each others for a long time. The Magellanic System moves in the gravitational potential of our Galaxy; it is exposed to ram pressure through its movement in the galactic halo. Both effects ought to be noticeable in their present structure and kinematics. It is generally assumed, but not definitely proven, that the Clouds have been bound to our Galaxy for at least the last 7 Gyr. Most models assume that the Clouds lead the Magellanic Stream. The interaction between the Clouds has influenced their structure and kinematics severely. The effects should be possible to trace in the motions of their stellar and gaseous components as pronounced disturbances. Recent astrometric contributions in this field show a great promise for the future if still higher accuracy can be achieved.

A Drag Dominated Model of the Magellanic Stream

1985 ◽  
Vol 6 (2) ◽  
pp. 195-198 ◽  
Author(s):  
Gerhardt R. Meurer ◽  
G. V. Bicknell ◽  
R. A. Gingold
Keyword(s):  
Magellanic Clouds ◽  
Radial Velocities ◽  
Tidal Model ◽  
Drag Forces ◽  
Wide Range ◽  
Magellanic Stream ◽  
Gaseous Halo ◽  
Gas Drag ◽  
Magellanic System

AbstractWe present here the best of a series of models of the Magellanic stream. The dominant force in these models is gas drag. Gaseous cloudlets are torn from the bridge between the Large and Small Magellanic Clouds as the Magellanic system passes through a hot gaseous halo about our galaxy. The cloudlets are then stretched apart from each other by tidal and drag forces to form the Magellanic stream. Our best model closely reproduces the position of the stream on the sky and the run of radial velocities along the Magellanic stream. The agreement is almost as good as the best purely tidal model. In our best model the Magellanic system is only loosely bound to our galaxy and is on the first encounter with it. This overcomes some of the problems with purely tidal models. Our series of models indicate that there is a wide range of parameters that will produce a reasonable stream under the forces of gas drag and gravity.

scholarly journals N-Body Simulations of the Magellanic System Including Gas Dynamics and Star Formation

1999 ◽  
Vol 186 ◽  
pp. 60-60
Author(s):  
A.M. Yoshizawa ◽  
M. Noguchi
Keyword(s):  
Star Formation ◽  
Gas Dynamics ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Small Magellanic Cloud ◽  
Tidal Distortion ◽  
Formation And Evolution ◽  
Magellanic Stream ◽  
Magellanic System

The system of the Magellanic Clouds is considered to be dynamically interacting among themselves and with our Galaxy. This interaction is thought to be the cause of many complicated features seen in the Magellanic Clouds and the Magellanic Stream (see Westerlund 1990, A&AR, 2, 27). In order to better understand the formation and evolution of the Magellanic System, we carry out realistic N-body simulations of the tidal distortion of the Small Magellanic Cloud (SMC) due to our Galaxy and the Large Magellanic Cloud (LMC).

scholarly journals A collision between the Large and Small Magellanic Clouds 2×108 years ago

1985 ◽  
Vol 106 ◽  
pp. 471-476
Author(s):  
M. Fujimoto ◽  
T. Murai
Keyword(s):  
Triple System ◽  
Gravitational Interaction ◽  
Magellanic Clouds ◽  
The Past ◽  
Model Galaxy ◽  
Binary State ◽  
The Galaxy ◽  
Magellanic Stream

A number of orbits are obtained for the Large and Small Magellanic Clouds (LMC and SMC) revolving around a model Galaxy with a massive halo. It is suggested that the SMC approached the LMC as close as 3 to 7 kpc about 200 million years ago, if these clouds have been in a binary state for the past 1010 years, and the Magellanic Stream (MS) is due to the gravitational interaction among the triple system of the Galaxy, LMC, and SMC.

scholarly journals The galactic wake model of the Magellanic Stream

1979 ◽  
Vol 84 ◽  
pp. 575-576
Author(s):  
Joel N. Bregman
Keyword(s):  
Galactic Plane ◽  
Magellanic Clouds ◽  
Radial Velocities ◽  
Tidal Model ◽  
Interaction Models ◽  
Self Consistent ◽  
Wake Model ◽  
Pass Through ◽  
Consistent Treatment ◽  
Magellanic Stream

Tidal interaction models for the origin of the Magellanic Stream have been fairly successful in reproducing the radial velocities of the Stream (Lin and Lynden-Bell 1977, Davies and Wright 1977). However, no investigator has yet attained a self consistent treatment in which (1) the LMC and SMC are bound for at least 5×109 yr, (2) the passing Magellanic Clouds warp the galactic plane, and (3) the Stream velocities are reproduced (Fujimoto and Sofue 1977). Also, Mathewson, Schwarz, and Murray (1977) argue that their 21 cm observations are evidence against the tidal model. To avoid these problems, they suggest that the Magellanic Clouds pass through a hot coronal gas and produce vortices in their wake which radiatively cool to form the HI clouds comprising the Stream.

The ‘High Velocity Cloud’ Origin of the Magellanic System

1987 ◽  
Vol 7 (1) ◽  
pp. 19-25 ◽  
Author(s):  
D. S. Mathewson ◽  
S. R. Wayte ◽  
V. L. Ford ◽  
K. Ruan
Keyword(s):  
High Velocity ◽  
Galactic Halo ◽  
Magellanic Clouds ◽  
The One ◽  
Magellanic Stream ◽  
Gaseous Halo ◽  
Velocity Cloud ◽  
High Velocity Cloud ◽  
Magellanic System

AbstractIt is believed that the splitting of the SMC into two fragments and the production of the Inter-Cloud gas and the Magellanic Stream occurred in the one event 4 × 108 years ago. This event was a collision between the LMC and SMC. This time is too short for the Stream to be tidal, or be the result of stripping of the Inter-Cloud gas by a diffuse gaseous halo. It is proposed that the clouds in the Stream are the results of collisions between the Inter-Cloud gas and HVCs in the Galactic halo. A model of this process accounts for all of the observational features of the Stream. Observations of HVCs in the path of the Magellanic Clouds are used to predict the development of the Stream. The HVCs in our halo are thought to be a result of a collision of a galaxy with our Galaxy 6 × 109 years ago.

scholarly journals The Magellanic Stream: theoretical considerations

1979 ◽  
Vol 84 ◽  
pp. 557-566 ◽  
Author(s):  
M. Fujimoto
Keyword(s):  
Local Group ◽  
Galactic Disk ◽  
Magellanic Clouds ◽  
Particle Simulation ◽  
The Past ◽  
Local Supercluster ◽  
New Models ◽  
The Galaxy ◽  
Magellanic Stream ◽  
Theoretical Considerations

The tidal and the primordial theories for the Magellanic Stream are examined in a frame of test-particle simulation for the interacting triple system of the Galaxy, the Large and Small Magellanic Clouds (LMC and SMC). Difficulties of the radial velocity of the Stream still beset these two theories. Several new models for the Stream and the Clouds are briefly discussed in relation to the bending of the galactic disk, the past binary orbits of the LMC and SMC and also the Local Group and the Local Supercluster of galaxies.

scholarly journals High-Resolution N-body Simulations of Galactic Cannibalism: The Magellanic Stream

2004 ◽  
Vol 21 (2) ◽  
pp. 222-227 ◽  
Author(s):  
Tim W. Connors ◽  
Daisuke Kawata ◽  
Sarah T. Maddison ◽  
Brad K. Gibson
Keyword(s):  
Phase Space ◽  
Galaxy Formation ◽  
Host Galaxy ◽  
Computational Power ◽  
Tidal Model ◽  
Dimensional Phase Space ◽  
History Of ◽  
Magellanic Stream ◽  
The Universe ◽  
Magellanic System

AbstractHierarchical clustering represents the favoured paradigm for galaxy formation throughout the Universe; due to its proximity, the Magellanic system offers one of the few opportunities for astrophysicists to decompose the full six-dimensional phase-space history of a satellite in the midst of being cannibalised by its host galaxy. The availability of improved observational data for the Magellanic Stream and parallel advances in computational power has led us to revisit the canonical tidal model describing the disruption of the Small Magellanic Cloud and the consequent formation of the Stream. We suggest improvements to the tidal model in light of these recent advances.

scholarly journals Models for the dynamical evolution of the Magellanic System

2008 ◽  
Vol 4 (S256) ◽  
pp. 105-116
Author(s):  
Kenji Bekki
Keyword(s):  
Galactic Halo ◽  
Dynamical Evolution ◽  
Magellanic Clouds ◽  
Young Stars ◽  
Proper Motions ◽  
Self Consistent ◽  
The Galaxy ◽  
Formation And Evolution ◽  
Magellanic Stream ◽  
Magellanic System

AbstractI 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.

scholarly journals The Magellanic Stream and its Related Problems

1984 ◽  
Vol 108 ◽  
pp. 115-123 ◽  
Author(s):  
M. Fujimoto ◽  
T. Murai
Keyword(s):  
Radial Velocity ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Optical Observations ◽  
Dark Halo ◽  
Small Magellanic Cloud ◽  
Characteristic Structure ◽  
Tidal Model ◽  
Space Orientation ◽  
Magellanic Stream

A brief survey is made of recent 21-cm and optical observations of the Magellanic Stream(MS). The space orientation of the Magellanic Clouds is touched upon in relation to modelling the MS. After summarizing a variety of models for the MS, we show that if our Galaxy is massive with a huge dark halo, a tidal model is most suitable for reproducing its characteristic structure and high-negative radial velocity. Past orbits of the Large and the Small Magellanic Cloud (LMC and SMC) are determined uniquely for the last 2×109 yr, if we postulate that the LMC and SMC are bound together for 1010 yr: Highly-noncircular motion of the SMC around the LMC could give a clue to understand some peculiar features associated with the Magellanic Clouds.

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