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Fig. 3.


Evolution of radial distribution of the mean stellar mass in the cluster models with eigenevolution (red lines are for non-segregated models and blue lines for segregated models). Each row of plots corresponds to one model (top and middle have 50% initial binaries but different pairing methods; the bottom row is with 100% initial binaries). Time increases from left to right in the units of the initial half-mass relaxation time.

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