Dynamics of Globular Clusters

  title={Dynamics of Globular Clusters},
  author={Lyman S. Spitzer},
  pages={465 - 472}
  • L. Spitzer
  • Published 3 August 1984
  • Physics, Medicine
  • Science
In their attempt to reach kinetic equilibrium, through gravitational encounters between separate stars, globular clusters are driven to destruction, with their cores collapsing and their outer regions expanding. The effects of core collapse, which apparently produces x-ray sources, are not yet fully understood, but white dwarfs and neutron stars, probably in binary systems, are thought to be involved, and possibly black holes as well. 

Topics from this paper

High resolution kinematics of galactic globular clusters. I
Integrated central velocity dispersions are presented for 7 globular clusters, three of which known to be post core-collapsed. The statistical significance of the measurements is discussed. For one
Long-Term Evolution of Cores of Globular Clusters after Core Collapse
Fluctuations play an important role in the post-collapse evolution of cores of globular clusters. We present a simple model for the long-term evolution of a globular cluster which includes a
Binaries in Globular Clusters
Binary stars in a globular cluster (hereafter, GC) may be primordial (i.e. formed along with the cluster), or the result of cluster dynamics. “Dynamical” binaries can result from conservative
Binary stars in a globular cluster (hereafter, GC) may be primordial (i.e. formed along with the cluster), or the result of cluster dynamics. “Dynamical” binaries can result from conservative
Surface photometry of globular clusters.
Much of what we know about the structure, dynamics, and evolution of globular clusters derives from their observed density profiles, and their interpretations. In this review, I will briefly describe
Primordial black holes in globular clusters
IT HAS recently been recognized1 that significant numbers of medium-mass black holes (of order 10 solar masses) should form in globular clusters during the early stages of their evolution. Here we
Dynamics of the globular cluster NGC 362
In this paper we have examined the internal dynamics of the globular cluster NGC 362 using a combination of V-band CCD images and echelle spectra of member red giants. A V-band surface brightness
Monte Carlo simulations of star clusters – II. Tidally limited, multimass systems with stellar evolution
A revision of Stodo lkiewicz's Monte Carlo code is used to simulate evolution of large star clusters. The new method treats each superstar as a single star and follows the evolution and motion of all
Star Clusters in Evolving Galaxies
Their ubiquity and extreme densities make star clusters probes of prime importance of galaxy evolution. Old globular clusters keep imprints of the physical conditions of their assembly in the early
A direct N-body model of core-collapse and core oscillations
We report on the results of a direct N-body simulation of a star cluster that started with N = 200000, comprising 195000 single stars and 5000 primordial binaries. The code used for the simulation


The dynamical evolution of globular clusters
The fundamental physical ideas underlying the dynamical behavior of globular star clusters are reviewed. The results of detailed numerical experiments involving large N-body stellar systems are
Computer Simulations of Stellar Systems
This review of numerical simulations concentrates mainly on collisional systems, that is, those whose age is greater than the time scale for significant orbital changes by encounter. Topics include
Is there life after core collapse in globular clusters
Theoretical arguments are given indicating that many dense globular clusters have already gone through core collapse and are now slowly expanding. The energy needed for this bounce is provided by
Random gravitational encounters and the evolution of spherical systems. III - Halo.
The accumulation of stars in the halo of a spherical stellar system, together with the escape of stars from the system, result from stellar encounters within a dense central core. The resultant halo
On formation of close binaries by two-body tidal capture
We calculate in detail the two-body tidal capture mechanism of Fabian, Pringle, and Rees: when two unbound stars have a close encounter, they may become bound by the energy that each deposits into
Effect of binary stars on the dynamical evolution of stellar clusters. II. Analytic evolutionary models
We use analytic models to compute the evolution of the core of a stellar system due simultaneously to stellar evaporation which causes the system (core) to contract and to its binaries which cause it
Exchange collisions between binary and single stars
In this paper we calculate the probability that existing binaries in various stellar systems have suffered exchange collisions with single stars. After such a collision the former single star is one
Monte Carlo models of star clusters
The dynamical evolution of spherical star clusters under the effect of internal encounters is followed numerically using a Monte Carlo procedure. Successive states of the system are computed,
X-ray evidence for white dwarf binaries in globular clusters
An apparently distinct class of low-luminosity (L/sub x/approx.10/sup 32/--10/sup 34/ ergs /sup -1/) X-ray sources has been discovered in globular clusters from a survey with the IPC detector on the
Numerical integration of the Fokker-Planck equation and the evolution of star clusters
A new numerical method for studying the evolution of spherical star clusters is presented. This method employs direct numerical integration of the orbit-averaged Fokker-Planck equation in