Evolution of star clusters after core collapse

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Abstract
A gaseous model is used to study the evolution (on a relaxation time-scale) of the core of a spherical cluster of identical stars. The system is enclosed in a distant adiabatic boundary, and the energy imparted by interaction with binaries (mainly in the core) is modeled by a simple analytical form. The results for the phase of the evolution which follows the initial collapse of the core are compared with those of other authors, and the qualitative differences which appeared in previous published results are reconciled. The post-collapse behavior is sometimes steady, but sometimes exhibits a linear instability which leads to the non-linear ‘gravothermal oscillations’ discovered by Sugimoto and Bettwieser. Results are presented which demonstrate the nature of these different behaviors.

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