Open AccessMonte Carlo simulations of star clusters – V. The globular cluster M4
Author(s) -
Heggie Douglas C.,
Giersz Mirek
Publication year - 2008
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2008.13702.x
Subject(s) - physics , globular cluster , astrophysics , blue straggler , star cluster , white dwarf , monte carlo method , mass segregation , velocity dispersion , cluster (spacecraft) , stellar evolution , stars , radius , astronomy , surface brightness , black hole (networking) , galaxy , statistics , mathematics , computer science , programming language , computer network , routing protocol , computer security , routing (electronic design automation) , link state routing protocol
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 12 Gyr 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: according to our model, 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. Finally, we 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.