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


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.