SCYON Abstract

Received on April 9 2002

Dynamical evolution of rotating stellar systems --
II. Post-collapse, equal mass system

AuthorsE. Kim (1,2), C. Einsel (1), H.M. Lee (1), R. Spurzem (2), M.G. Lee (1)
Affiliation1 Astronomy Program, SEES, Seoul Nat. Univ., Seoul 151-742, Korea
2 Astronomisches Rechen-Institut, Mönchhofstrasse 12-14, 69120 Heidelberg, Germany
Accepted byMonthly Notices of the Royal Astronomical Society
Contactspurzem@ari.uni-heidelberg.de
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Abstract

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 (1999), 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 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.