Stability of star clusters as galactic satellites. III Preliminary applications to the system of the globular clusters

Details Stability of star clusters as galactic satellites. III Preliminary applications to the system of the globular clusters Stability of star clusters as galactic satellites. III Preliminary applications to the system of the globular clusters

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...138..396a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 138, no. 2, Sept. 1984, p. 396-403.

Astronomy and Astrophysics

Astrophysics

3

Dwarf Stars, Mass Distribution, Natural Satellites, Star Clusters, Stellar Motions, Astronomical Models, Dynamic Stability, Galactic Mass, Globular Clusters, Space Density

Scientific paper

Various theoretical approaches to analyzing the linear stability of stellar motions in a spherically symmetric satellite orbiting a point-mass galaxy are discussed and compared with observational data. The orbiting object could be a globular cluster or dwarf spheroidal galaxy. The radius of the satellite is assumed to be limited by the requirements of a uniform mass density. Clusters lie along a transition curve separating regions of stability and instability with regard to galactic tidal forces. It is found that the linear stability analysis is in agreement with a previous model for the limiting radius being 2/3 of King's tidal radius. The radius criterion is used to select standard values for the galactic rotation curve, the solar galactocentric distance (SGD), the mass within the SGD, the galactic mass, etc. Predictions of several simple galactic models are then compared with data on 102 globular clusters. It is found that a point-mass model is unacceptable for the Galaxy, and galactic satellite dynamics can be treated in terms of a galactic mass density that is proportional to the inverse square of the galactic radius.

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