2007/09/27 by Eunhyeuk Kim, E. Kim, I. Yoon +5 · 59 citations
Physics and Astronomy · #Acceleration #Angular acceleration #Angular momentum #Angular velocity #Cluster (spacecraft) #Pulsars and Gravitational Waves Research #Specific relative angular momentum #Star cluster #Stars #Statistical Mechanics and Entropy #Stellar, planetary, and galactic studies #Total angular momentum quantum number #Velocity dispersion #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2007.12524.x
published in Monthly Notices of the Royal Astronomical Society 383(1), 2-10 (Oxford University Press) · 11 pages, 13 eps figures, accepted for the publication of MNRAS
arxiv created 2007/09/27 · openalex publication_date 2007/11/28 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We have carried out N-body simulations for rotating star clusters with equal mass and compared the results with Fokker–Planck models. These two different approaches are found to produce fairly similar results, although there are some differences with regard to the detailed aspects. We confirmed the acceleration of the core collapse of a cluster due to an initial non-zero angular momentum and found a similar evolutionary trend in the central density and velocity dispersion in both simulations. The degree of acceleration depends on the initial angular momentum. Angular momentum is being lost from the cluster due to the evaporation of stars with a large angular momentum on a relaxation time-scale.