Dynamical evolution of rotating stellar systems - II. Post-collapse, equal mass system
arXiv:astro-ph/0109062 · doi:10.1046/j.1365-8711.2002.05420.x
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.
12 pages (MNLaTeX), 17 Postscript figures, Submitted to MNRAS
References in corpus (23)
- The dynamical evolution of massive black hole binaries - I. Hardening in a fixed stellar background
- The Evolution of Globular Clusters in the Galaxy
- Effects of Tidal Shocks on the Evolution of Globular Clusters
- Statistics of N-body Simulations I. Equal Masess Before Core Collapse
- Scaling of N-body calculations
- Direct N-body Modelling of Stellar Populations: Blue Stragglers in M67
- Monte-Carlo Simulations of Globular Cluster Evolution - I. Method and Test Calculations
- Statistics of N-Body Simulations. III. Unequal Masses
- Monte Carlo Simulations of Globular Cluster Evolution - II. Mass Spectra, Stellar Evolution and Lifetimes in the Galaxy
- The time-scale for core collapse in spherical star clusters
- Post-Collapse evolution of globular clusters
- Basic N-Body Modelling of the Evolution of Globular Clusters. I. Time Scaling
- Monte Carlo simulations of star clusters - II. Tidally limited, multi-mass systems with stellar evolution
- Comparing Direct N-Body Integration with Anisotropic Gaseous Models of Star Clusters
- Statistics of N-Body Simulations. II. Equal Masses after Core Collapse
- Direct collisional simulation of 10 000 particles past core collapse
- A stochastic Monte Carlo approach to model real star cluster evolution, II. Self-consistent models and primordial binaries
- Fabry-Perot Measurements of the Dynamics of Globular Cluster Cores: M15 (NGC~7078)
- Fokker-Planck Models of Star Clusters with Anisotropic Velocity Distributions. II. Post-Collapse Evolution
- Fokker-Planck Models of Star Clusters with Anisotropic Velocity Distributions. III. Multi-Mass Clusters
- Evolution of Tidally Truncated Globular Clusters with Anisotropy
- Evolution of Multi-mass Globular Clusters in Galactic Tidal Field with the Effects of Velocity Anisotropy
- The disruption of globular star clusters in the galaxy: A comparative analysis between Fokker-Planck and N-body models
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- Formation of Massive Black Holes in Dense Star Clusters. I. Mass Segregation and Core Collapse
- Relativistic Binaries in Globular Clusters
- A new Monte Carlo code for star cluster simulations: II. Central black hole and stellar collisions
- Electromagnetic Counterparts to Massive Black Hole Mergers
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- Gravitational Radiation from Intermediate-Mass Black Holes
- N-body Models of Rotating Globular Clusters
- Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. V. The rapid rotation of 47 Tuc traced and modeled in three dimensions
- Differences in the rotational properties of multiple stellar populations in M 13: a faster rotation for the "extreme" chemical subpopulation
- Rotation in young massive star clusters
- Monte Carlo Simulations of Star Clusters - V. The globular cluster M4
- A stochastic Monte Carlo approach to model real star cluster evolution, III. Direct integrations of three- and four-body interactions
- The VLT-FLAMES Tarantula Survey VI: Evidence for rotation of the young massive cluster R136
- Star Clusters in Evolving Galaxies
- Self-consistent models of quasi-relaxed rotating stellar systems
- Gravitating discs around black holes
- Comparative study between N-body and Fokker-Planck simulations for rotating star clusters - II. 2-component models
- Comparative study between N-body and Fokker-Planck simulations for rotating star clusters: I. Equal-mass system
- A stochastic Monte Carlo approach to model real star cluster evolution, II. Self-consistent models and primordial binaries
- Dynamical Evolution of Rotating Stellar Systems: III. The Effect of Mass Spectrum
- Kinematical evolution of tidally limited star clusters: rotational properties
- 2D Fokker-Planck models of rotating clusters
- The dynamical fate of binary star clusters in the Galactic tidal field
- Monte Carlo simulations of star clusters -- III. A million body star cluster
- The impact of stellar evolution on rotating star clusters: the gravothermal-gravogyro catastrophe and the formation of a bar of black holes
- The role of rotation on the formation of second generation stars in globular clusters
- New insights into star cluster evolution towards energy equipartition
- Mass Segregation and Tidal Tails of the Globular Cluster NGC 7492
- Effects of External Tidal Field on the Evolution of Multi-mass Star Clusters
- Hyades dynamics from N-body simulations: Accuracy of astrometric radial velocities from Hipparcos
- Early dynamical evolution of rotating star clusters in a tidal field
- Relativistic Binaries in Globular Clusters
- Anisotropic Mass Segregation in Rotating Globular Clusters
- Mass segregation and dynamics of primordial binaries in star clusters with a radially anisotropic velocity distribution
- Anisotropic gaseous models of tidally limited star clusters -- comparison with other methods
- Dynamics of star clusters with tangentially anisotropic velocity distribution
- The Formation of Binary Star Clusters in the Milky Way and Large Magellanic Cloud
- Supermassive Black Holes in Galactic Nuclei with Tidal Disruption of Stars: Paper II - Axisymmetric Nuclei
- Higher order moment models of dense stellar systems: Applications to the modeling of the stellar velocity distribution function
- Solving procedure for a twenty-five diagonal coefficient matrix: direct numerical solutions of the three dimensional linear Fokker-Planck equation
- The internal line-of-sight kinematics of NGC 346: the rotation of the core region
- Evolution of star clusters with initial bulk rotation via N-body simulations
- Dynamical Processes in Globular Clusters
- Non-resonant relaxation of rotating globular clusters
- Direct N-body simulations of rotating and extremely massive Population III star clusters
- Right round: onset and long-term evolution of rotation in star clusters
- Evolution towards energy equipartition in star clusters: effects of the tidal field, primordial binaries, and internal velocity anisotropy