Abstract
We present here some recent (and very preliminary) finding from a study of the stages of the post-core-collapse evolution of an isolated cluster of identical point “stars”. The method used to follow the behavior of the system is the unified N-body/statistical treatment described in detail by McMillan and Lightman (1984a) and by Lightman and McMillan elsewhere in this volume. Briefly, the method combines the standard “large-N” and “small-N” approaches to the problem in the régimes where they are appropriate by treating the inner regions (r < rN) exactly with a regularized Aarseth N-body code (Aarseth, 1972), while permitting stars at greater and greater radii to retain less and less of their individual identities, ultimately treating the outer portions of the system (r > KrN) in an almost purely statistical fashion.
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References
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© 1985 International Astronomical Union
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McMillan, S.L.W. (1985). The Early Stages of Post-Collapse Cluster Evolution. In: Goodman, J., Hut, P. (eds) Dynamics of Star Clusters. International Astronomical Union. Symposium, vol 113. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-5335-2_39
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DOI: https://doi.org/10.1007/978-94-009-5335-2_39
Publisher Name: Springer, Dordrecht
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