Tidal evolution of globular clusters. II - The effects of Galactic tidal field and diffusion

Details Tidal evolution of globular clusters. II - The effects of Galactic tidal field and diffusion Tidal evolution of globular clusters. II - The effects of Galactic tidal field and diffusion

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...386..519o&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 386, Feb. 20, 1992, p. 519-538. Research supported by University of Califor

Statistics

Computation

61

Celestial Mechanics, Diffusion, Galactic Evolution, Globular Clusters, Stellar Motions, Tides, Angular Momentum, Astronomical Models, Computational Astrophysics, Milky Way Galaxy, Radial Velocity

Scientific paper

The tidal evolution of globular clusters subject to various degrees of the internal diffusion process is investigated. In cases of negligible diffusion, clusters are found to be tidally truncated to the theoretical tidal radius at perigalacticon. There is no apparent orbital phase dependence of the tidal radius for clusters with eccentric orbits. In clusters with moderately short two-body relaxation time scales, diffusion processes significantly modify the structure of the outer regions in such a way that the limiting radius may be comparable to the tidal radius at apogalacticon. The Galactical tidal torque induces isotropy in the velocity dispersion of the outer regions of the cluster. For relaxed clusters, the velocity dispersion may be isotropic in the core, anisotropic in the envelope and isotropic near the limiting radius. Disk shocking is also very efficient for isotropizing the orbits of stars in the outer cluster regions. Stars with direct orbits are less stable, so that prolonged tidal interaction can lead to apparent retrograde rotation in the outer regions of the cluster.

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