Star clusters containing massive, central black holes. IV - Galactic tidal fields
Abstract
Monte Carlo simulations of star cluster evolution were used to investigate the effects of a central black hole and/or galactic tidal field on a cluster. The tidal field is introduced by incorporating a tidal radius and allowing for tidal stripping of halo stars. It is found that the late phases of cluster evolution are characterized by homologous core collapse agreeing well with models based on gravothermal instability and the 1 + 1 Fokker-Planck calculations, and by significant velocity anisotropy persisting over a substantial fraction of the outer mass of the system but significant at progressively smaller radii as the collapse proceeds. Cluster evolution with central black hole is independent of when the hole is introduced. The core collapse is eventually halted by heat flux due to stellar consumption by the hole, causing the reexpansion of the cluster until a quasi-stationary state is attained. The finite tidal radius largely does not affect the late stages of core evolution.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- February 1982
- DOI:
- 10.1086/159691
- Bibcode:
- 1982ApJ...253..921D
- Keywords:
-
- Black Holes (Astronomy);
- Globular Clusters;
- Stellar Evolution;
- Supermassive Stars;
- Collapse;
- Galactic Structure;
- Monte Carlo Method;
- Astrophysics