Open AccessDynamical evolution of rotating stellar systems – II. Post‐collapse, equal‐mass system
Author(s) -
Kim E.,
Einsel C.,
Lee H. M.,
Spurzem R.,
Lee M. G.
Publication year - 2002
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2002.05420.x
Subject(s) - physics , fokker–planck equation , astrophysics , classical mechanics , star cluster , kinematics , binary number , stellar evolution , stellar dynamics , mass distribution , orbit (dynamics) , gravitational collapse , computational astrophysics , binary star , star (game theory) , star formation , mechanics , stability (learning theory) , stars , galaxy , differential equation , arithmetic , mathematics , quantum mechanics , aerospace engineering , machine learning , computer science , engineering
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.