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The Evolution of the System of Globular Clusters

Published online by Cambridge University Press:  19 July 2016

Jeremiah P. Ostriker
Jeremiah P. Ostriker*
Affiliation:
Princeton University Observatory

Extract

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Globular clusters have a sufficiently distinct character that we can treat the system of globular clusters, as a distinct object which has a size, mass and angular momentum, but also, an internal density distribution, velocity distribution, and, in general, a detailed interior structure. Shapley, of course, pioneered in the effort to model, that is to describe, the existing state of the system from our vantage point. At the present time we probably have an inventory of clusters which is largely complete, and for the majority of the identified systems we have good knowledge (cf for example Webbink, 1985) of positions in the galaxy, one component of galactic velocity and a sufficiently detailed picture of the interior dynamical state to characterize each cluster by a luminosity and two radii: a core radius rc where the surface density has fallen to half the central value, and a tidal radius rt determined by a fit to the King (1966) truncated isothermal profiles, which is thought to represent the radius beyond which the tidal force due to the galaxy effectively exceeds the force due to the clusters own gravity.

Type
Chapter IV. Review Papers on Evolution of Globular Clusters
Information
Symposium - International Astronomical Union , Volume 126: The Harlow-Shapley Symposium on Globular Cluster Systems in Galaxies , 1988 , pp. 271 - 281
Copyright
Copyright © Kluwer 1988 

References

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