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tokens: effects of binary disruption and binary segregation resulting in a significant delay of complete mixing compared to the inert binary case. In order to further describe the overall effect of the different dynamical processes affecting the survival and evolution of binaries on the FG and SG binary mixing, we present in Fig. 3 the time evolution of the cumulative radial distribution of FG and SG binaries for four different models with different values of the initial hardness parameter of the binary population. Figure 3. Cumulative radial distribution of FG (red lines) and SG (blue lines) binaries. From left to right, each panel shows the evolution of radial distribution. Three different models with x g,0 = 3, 3-20, 50, and 800 are presented (top to bottom). The cumulative radial distribution of inert binaries are shown as dashed lines for comparison. The last panel for the model with x g,0 = 800, the distribution at t ∼ 40τ rh, 0 is shown to illustrate a complete spatial mixing of very compact binaries. The cumulative radial distribution of FG and SG inert binaries in the MPr5f1m2 are also shown in order to illustrate the spatial mixing of stars with the same mass of binaries but not affected by other processes such as ionization and ejection due to the recoil velocity acquired during interactions with other stars. At t = 0, FG and SG binaries in all models have the same cumulative distribution. For the MPr5f1x3 model, the rapid disruption of SG binaries significantly depletes the inner binary population as illustrated by the shift of the SG binary cumulative radial distribution towards the outer regions. For the MPr5f1x3-20 model, the evolution of the distribution of FG binaries is similar to that for the MPr5f1x3 model. However, the presence of harder binaries implies that the effects of ionization are not as strong as in the previous case and the evolution of the SG cumulative radial distribution is more similar to that of inert binaries. It is interesting to note the development of an approximately flat portion in the cumulative radial distribution of SG binaries in the MPr5f1x3 and x3-20 simulations. The formation of this shell depleted in SG binaries is due to the combined effect of binary segregation and disruption; binaries are rapidly disrupted in the inner regions but as the segregation time-scale increases with the distance from the cluster’s centre. Therefore, there is no replenishment of binaries beyond the gap because the segregation time-scale is longer than the cluster’s age (see also the fig. 7 in Paper I ). The development of this gap is also responsible for the rapid variation in R h,SG and R h,FG / R h,SG around t ∼ 23τ rh, 0 in Figs 1 and 2 for the MPr5f1x3-20. For the MPr5f1x800 model, the cumulative distributions for FG and SG binaries are, in general, very similar to those in the inert binary model. Eventually, the spatial mixing of FG and SG binaries is achieved at t ∼ 40τ rh, 0 . Fig. 4 shows the time evolution of the