Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...442..142o&link_type=abstract
The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 442, no. 1, p. 142-158
Astronomy and Astrophysics
Astronomy
131
Dark Matter, Disrupting, Dwarf Galaxies, Gravitational Effects, Local Group (Astronomy), Mathematical Models, Milky Way Galaxy, Angular Momentum, Density Distribution, Equations Of Motion, Magellanic Clouds, Many Body Problem, Star Distribution, Velocity Distribution
Scientific paper
The Milky Way induces a strong tidal perturbation on its satellite dwarf spheroidal galaxies. We present numerical simulations of tidal interactions between these low-density dwarf spheroidal galaxies and the Milky Way. Our results indicate that dwarf spheroidal galaxies with limiting radius much larger than the theoretical tidal radius are unstable and likely to be tidally disrupted on a Hubble-time. However, dwarf spheroidal galaxies can survive over a Hubble time if their limiting radii are less than twice their tidal radii at perigalacticon. In a galaxy which is undergoing tidal disruption, (1) the projected surface density is flattened in the galaxy's orbital plane and follows a power-law distribution from the galaxy's center, (2) the velocity dispersion is sustained at the current virial equilibrium value, and (3) the central density ofthe residual remnant is maintained even after most of the initial mass is lost. Beyond the tidal radius, the escapers have a radial velocity gradient along the azimuthal direction of the galaxy's motion. When compared with observational data, our theoretical results are consistent with the scenarios that (1) some dwarf spheroidal galaxies contain dark matter, and (2) some dwarf spheroidal galaxies may be part of the debris that was tidally torn from the Large Magellanic Cloud (LMC) by the Galaxy.
Aarseth Sverre J.
Lin Doug N. C.
OH Suhk Kun
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