Tidal models of the Magellanic system
Abstract
The role of tidal interactions in the evolution of the LMC, the SMC, and the Magellanic Stream (MS) is investigated by means of model computations. The problems posed by the observational constraints and not solved by the models of Lin and LyndenBell (1982) or Murai and Fujimoto (1981) are reviewed, and results for simulations involving testparticle disks, selfgravitating disks, and selfgravitating bars in parabolic orbits with respect to the Galaxy (assuming that the LMC is at or near its 50kpc perigalacticon at present and that the SMC and LMC are far enough apart that no immediate tidal interaction occurs) are presented graphically. The bar calculations produce streams with the correct orientation (but not the correct velocities) and predict LMCSMC approaches to within 10 kpc within the last 300 Myr as well as the nonsurvival of the Magellanic system as a bound pair. The number and seriousness of the problems facing these tidal models with regard to the MS are indicated, and nontidal explanations such as that of Mathewson et al. (1977) are briefly considered.
 Publication:

Proceedings of the Astronomical Society of Australia
 Pub Date:
 1984
 DOI:
 10.1017/S1323358000017343
 Bibcode:
 1984PASAu...5..469G
 Keywords:

 Astronomical Models;
 Gravitational Effects;
 Magellanic Clouds;
 Tides;
 Milky Way Galaxy;
 Radial Velocity;
 Star Distribution;
 Turbulent Wakes;
 Astrophysics