Monte Carlo Simulations of Star Clusters - V. The globular cluster M4
arXiv:0801.3968 · doi:10.1111/j.1365-2966.2008.13407.x
Abstract
We describe Monte Carlo models for the dynamical evolution of the nearby globular cluster M4. The code includes treatments of two-body relaxation, three- and four-body interactions involving primordial binaries and those formed dynamically, the Galactic tide, and the internal evolution of both single and binary stars. We arrive at a set of initial parameters for the cluster which, after 12Gyr of evolution, gives a model with a satisfactory match to the surface brightness profile, the velocity dispersion profile, and the luminosity function in two fields. We describe in particular the evolution of the core, and find that M4 (which has a classic King profile) is actually a post-collapse cluster, its core radius being sustained by binary burning. We also consider the distribution of its binaries, including those which would be observed as photometric binaries and as radial-velocity binaries. We also consider the populations of white dwarfs, neutron stars, black holes and blue stragglers, though not all channels for blue straggler formation are represented yet in our simulations.
arXiv comment10 pages, 13 figures. Some numbers and figures may change slightly before journal submission
References in corpus (31)
- Evolution of binary stars and the effect of tides on binary populations
- Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity
- Internal Dynamics of Globular Clusters
- The Evolution of Globular Clusters in the Galaxy
- HST color-magnitude diagrams of 74 galactic globular clusters in the HST F439W and F555W bands
- A Complete N-body Model of the Old Open Cluster M67
- High Resolution X-ray Imaging of a Globular Cluster Core: Compact Binaries in 47Tuc
- Statistics of N-body Simulations I. Equal Masess Before Core Collapse
- Scaling of N-body calculations
- Monte-Carlo Simulations of Globular Cluster Evolution - I. Method and Test Calculations
- Ground-Based CCD Astrometry with Wide Field Imagers. I. [Observations just a few years apart allow decontamination of field objects from members in two Globular clusters.]
- Monte Carlo Simulations of Globular Cluster Evolution. IV. Direct Integration of Strong Interactions
- Ground-based CCD astrometry with wide field imagers. II. A star catalogue for M67: [email protected] MPG/ESO astrometry, FLAMES@VLT radial velocities
- Statistics of N-Body Simulations. III. Unequal Masses
- The CFHT Open Star Cluster Survey. IV. Two Rich, Young Open Star Clusters: NGC 2168 (M35) and NGC 2323 (M50)
- Ratios of star cluster core and half-mass radii: a cautionary note on intermediate-mass black holes in star clusters
- A comprehensive Nbody study of mass segregation in star clusters: Energy equipartition and escape
- Monte Carlo simulations of star clusters - II. Tidally limited, multi-mass systems with stellar evolution
- Dynamical evolution of rotating stellar systems - II. Post-collapse, equal mass system
- HST Astrometry of M4 and the Galactic Constant V_0/R_0
- Statistics of N-Body Simulations. II. Equal Masses after Core Collapse
- Color--Magnitude Diagram and Luminosity Function of M4 Near the Hydrogen-Burning Limit
- A stochastic Monte Carlo approach to model real star cluster evolution, III. Direct integrations of three- and four-body interactions
- Dynamical Evolution of Rotating Stellar Systems: III. The Effect of Mass Spectrum
- Monte Carlo simulations of star clusters -- III. A million body star cluster
- Modest-2: A Summary
- Proper motion measurements as indicators of binarity in open clusters
- A Simple Dynamical Model for Omega Cen
- Radial Color Gradient and Main Sequence Mass Segregation in M30 (NGC 7099)
- NGC 6397: A case study in the resolution of post-collapse globular cluster cores
- McScatter: a Simple Three-Body Scattering Package with Stellar Evolution
Cited by in corpus (47)
- The Dynamical Evolution of Stellar Black Holes in Globular Clusters
- Compact Binaries in Star Clusters I - Black Hole Binaries Inside Globular Clusters
- Relativistic Binaries in Globular Clusters
- MOCCA Code for Star Cluster Simulations - II. Comparison with N-body Simulations
- MOCCA code for star cluster simulations - I. Blue Stragglers, first results
- Retention of Stellar-Mass Black Holes in Globular Clusters
- Modeling Dense Star Clusters in the Milky Way and Beyond with the Cluster Monte Carlo Code
- MOCCA-SURVEY Database I. Unravelling black hole subsystems in globular clusters
- Monte Carlo Simulations of Globular Cluster Evolution. V. Binary Stellar Evolution
- An Analytic Technique for Constraining the Dynamical Origins of Multiple Star Systems Containing Merger Products
- Multiple populations in globular clusters: the distinct kinematic imprints of different formation scenarios
- Monte Carlo Simulations of Star Clusters - VII. The globular cluster 47 Tuc
- Evolution of the Binary Fraction in Dense Stellar Systems
- Preparing the next gravitational million-body simulations: Evolution of single and binary stars in Nbody6++GPU, MOCCA and McLuster
- Compact Binaries in Star Clusters II - Escapers and Detection Rates
- The state of globular clusters at birth II: primordial binaries
- Star Clusters in Evolving Galaxies
- MOCCA-SURVEY database I. Accreting white dwarf binary systems in globular clusters -- IV. cataclysmic variables -- properties of bright and faint populations
- MOCCA Survey Database I: Dissolution of tidally filling star clusters harbouring BH subsystems
- Monte Carlo Simulations of Star Clusters - VI. The globular cluster NGC 6397
- Towards an N-body Model for the Globular Cluster M4
- Stellar Escape from Globular Clusters. I. Escape Mechanisms and Properties at Ejection
- MOCCA code for star cluster simulations - III. Stellar-mass black holes in the globular cluster M22
- Great Balls of FIRE II: The evolution and destruction of star clusters across cosmic time in a Milky Way-mass galaxy
- MOCCA-SURVEY database I. Accreting white dwarf binary systems in globular clusters -- I. cataclysmic variables -- present-day population
- 1Gyr in the Life of the Globular Cluster NGC 6397
- Dynamical Formation of Cataclysmic Variables in Globular Clusters
- Discovery of a double Blue Straggler sequence in M15: new insight into the core-collapse process
- Expansion Techniques for Collisionless Stellar Dynamical Simulations
- Dynamical modelling of globular clusters: challenges for the robust determination of IMBH candidates
- MOCCA: Dynamics and evolution of binary stars of multiple stellar populations in tidally filling and underfilling globular star clusters
- Finding Black Holes with Black Boxes -- Using Machine Learning to Identify Globular Clusters with Black Hole Subsystems
- Is there a Size Difference between Red and Blue Globular Clusters?
- On the absence of symbiotic stars in globular clusters
- Self-consistent simulations of star cluster formation from gas clouds under the influence of galaxy-scale tidal fields
- Close stellar encounters at the Galactic Centre I: The effect on the observed stellar populations
- Rapid formation of a very massive star >50000 and subsequently an IMBH from runaway collisions. Direct N-body and Monte Carlo simulations of dense star clusters
- Testing multi-mass dynamical models of star clusters with real data: mass segregation in three Galactic globular clusters
- GalevNB: a conversion from N-BODY simulations to observations
- The M4 Core Project with HST --- I. Overview and First-Epoch
- The initial conditions of observed star clusters - I. Method description and validation
- Higher order moment models of dense stellar systems: Applications to the modeling of the stellar velocity distribution function
- MOCCA-SURVEY Database -- I. Tidal disruption events of white dwarfs in globular clusters and young massive clusters
- Evolution of star clusters on eccentric orbits: semi-analytical approach
- Population Synthesis of Gravitational Wave Sources
- Gravitational Microlensing Rates in Milky Way Globular Clusters
- Is the overconcentration of pristine populations in Galactic globular clusters real? An N-body approach to the problem