Open AccessStar cluster ecology – V. Dissection of an open star cluster: spectroscopy
Author(s) -
Portegies Zwart Simon F.,
Hut Piet,
McMillan Stephen L. W.,
Makino Junichiro
Publication year - 2004
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.1365-2966.2004.07709.x
Subject(s) - physics , astrophysics , open cluster , pleiades , star cluster , stars , stellar evolution , stellar dynamics , astronomy , stellar mass , cluster (spacecraft) , mass segregation , radius , galaxy , star formation , binary star , computer science , programming language , computer security
We have modelled in detail the evolution of rich open star clusters such as NGC 2516, NGC 2287, Pleiades, Praesepe, Hyades, NGC 2660 and 3680, using simulations that include stellar dynamics as well as the effects of stellar evolution. The dynamics is modelled via direct N ‐body integration, while the evolution of single stars and binaries is followed through the use of fitting formulae and recipes. The feedback of stellar and binary evolution on the dynamical evolution of the stellar system is taken into account self‐consistently. Our model clusters dissolve in the tidal field of the Galaxy in a time‐span of the order of a billion years. The rate of mass loss is rather constant, ∼1 M ⊙ per million years. The binary fraction at first is nearly constant in time, then increases slowly near the end of a cluster's lifetime. For clusters which are more than about 10 8 yr old the fractions of stars in the form of binaries, giants and merger products in the inner few core radii are considerably higher than in the outer regions, beyond the cluster's half‐mass radius. When stars with masses ≳2 M ⊙ escape from the cluster, they tend to do so with velocities higher than average. The stellar merger rate in our models is roughly one per 30 million years. Most mergers are the result of unstable mass transfer in close binaries (∼70 per cent), but a significant minority are caused by direct encounters between single and binary stars. While most mergers occur within the cluster core, even beyond the half‐mass radius stellar mergers occasionally take place. We notice a significant birth rate of X‐ray binaries, most containing a white dwarf as the mass acceptor. We also find one high‐mass X‐ray binary with a neutron‐star accretor. If formed and retained, black holes participate in many (higher‐order) encounters in the cluster centre, resulting in a large variety of exotic binaries. The persistent triple and higher‐order systems formed in our models by dynamical encounters between binaries and single stars are not representative for the multiple systems observed in the Galactic disc. We conclude that the majority of multiples in the disc probably formed when the stars were born, rather than through later dynamical interactions.