Abstract
ABSTRA C T We present the first post-core-collapse models of initially rotating star clusters, using the numerical solution of an orbit-averaged 2D Fokker ‐ Planck equation. Based on the code developed by Einsel & Spurzem, we have improved the speed and the stability and included the steady three-body binary heating source. We have confirmed that rotating clusters, whether they are in a tidal field or not, evolve significantly faster than non-rotating ones. Consequences for the observed shapes, density distribution and kinematic properties of young and old star clusters are discussed. The results are compared with gaseous and 1D Fokker‐ Planck models in the non-rotating case.
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