Evolution of n-body open clusters

Details Evolution of n-body open clusters Evolution of n-body open clusters

Jan 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.224..193t&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 224, Jan. 1, 1987, p. 193-225. Research supported by No

Astronomy and Astrophysics

Astronomy

140

Fokker-Planck Equation, Many Body Problem, Open Clusters, Stellar Evolution, Stellar Mass, Density Distribution, Equations Of Motion, Solar Neighborhood, Velocity Distribution

Scientific paper

Using Aarseth's (1986) n-body code, simulations of the evolution of open clusters (containing as many as 1000 members) during long periods of time are discussed, and the effects of galactic tidal field, mass loss due to stellar evolution, and transient tidal shocks produced by passing interstellar clouds are included. Good agreement is found between the distribution of lifetime for galactic clusters and the life of the models. Tidal heating shapes the cluster halo, producing a distinctive density and velocity distribution, and encounters with standard clouds are shown not to alter the lifetime of the clusters. The effects of mass segregation and preferential escape of light stars can account for the depletion of low luminosity stars noted in the better studied central region of clusters.

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