Astronomy and Astrophysics – Astrophysics
Scientific paper
1995-06-30
Astronomy and Astrophysics
Astrophysics
20 pages, plain tex, figures available from d.c.heggie@ed.ac.uk; submitted to MNRAS
Scientific paper
We describe results from large numbers of $N$-body simulations containing from $250$ to $1000$ stars each. The distribution of stellar masses is a power law, and the systems are isolated. While the collapse of the core exhibits the expected segregation of different masses, we find that the post-collapse evolution is, at a first approximation, homologous. This is quite surprising because there is no reason for supposing that mass segregation should not continue to have a substantial effect on the evolution of the cluster. In fact the spatial distribution of the mean stellar mass is nearly static throughout the post-collapse regime, except for the overall expansion of the systems, and this helps to explain why the post-collapse evolution is nearly self-similar. Self-similarity is also exhibited by the distribution of anisotropy and the profile of departures from equipartition, which show little change during the post-collapse phase. The departures from energy equipartition and isotropy are small in the core and increase with radius. During post-collapse evolution massive stars (mainly) are removed from the system by binary activity. This effect dominates the preferential escape of low-mass stars due to standard two-body relaxation processes.
Giersz Mirek
Heggie Douglas C.
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