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The interplay of rotation and relaxation in star clusters and galactic nuclei

Published online by Cambridge University Press:  26 May 2016

R. Spurzem ,
E. Kim  and
H.M. Lee
R. Spurzem
Affiliation:
Astronomisches Rechen-Institut, Mönchhofstrasse 12-14, 69120 Heidelberg, Germany
E. Kim
Affiliation:
Dept. of Astronomy, Seoul Nat. Univ., Seoul 151-742, Korea
H.M. Lee
Affiliation:
Dept. of Astronomy, Seoul Nat. Univ., Seoul 151-742, Korea Institute of Space and Astronautical Science, Sagamihara, Japan

Abstract

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The impact of rotation on the relaxational dynamics of dense stellar systems is reviewed; while in the past linear stability analysis and a few N-body models existed only, we report recent advances in the technique of 2D Fokker-Planck models for axisymmetric rotating star cluster, now extending into the post-core collapse phase. It is confirmed that rotating clusters, whether they are in a tidal field or not, evolve significantly faster in pre-collapse than non-rotating ones, while in post-collapse only those in a tidal field keep their larger speed of evolution. Consequences for observed shapes, density distribution, and kinematic properties of young and old star clusters are discussed.

Type
Star Clusters
Information
Symposium - International Astronomical Union , Volume 208: Astrophysical Supercomputing using Particle Simulations , 2003 , pp. 93 - 102
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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