Monte Carlo simulations of star clusters - VI. The globular cluster NGC 6397

Mirek Giersz, Douglas C. Heggie

Research output: Contribution to journalArticlepeer-review

Abstract

We describe Monte Carlo models for the dynamical evolution of the nearby globular cluster NGC6397. The code includes treatments of two-body relaxation, most kinds of 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 12 Gyr of evolution, gives a model with a fairly satisfactory match to the surface brightness profile, the velocity dispersion profile and the luminosity function in two fields. We describe in particular those aspects of the evolution which distinguish this cluster from M4, which has a roughly similar mass and Galactocentric distance, but a qualitatively different surface brightness profile. Within the limitations of our modelling, we conclude that the most plausible explanation for the difference is fluctuations: both clusters are post-collapse objects, but sometimes have resolvable cores and sometimes not.

Original languageEnglish
Pages (from-to)1173-1183
Number of pages11
JournalMonthly Notices of the Royal Astronomical Society
Volume395
Issue number2
DOIs
Publication statusPublished - 11 May 2009

Keywords

  • stellar dynamics
  • methods: numerical
  • globular clusters: individual: NGC 6397
  • globular clusters: individual: M4
  • DEEP ADVANCED CAMERA
  • SPACE-TELESCOPE OBSERVATIONS
  • SURFACE-BRIGHTNESS PROFILES
  • DWARF COOLING SEQUENCE
  • POST-CORE-COLLAPSE
  • LOW-MASS STARS
  • BLACK-HOLES
  • STELLAR-SYSTEMS
  • MAIN-SEQUENCE
  • WHITE-DWARFS

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