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Fig. 5.

image

Distribution of the semi-major axis of the binary population for the set of simulations listed in Table 1. The data clearly shows that increasing the mass of the external potential the formed binaries tend to be more tightly bound. Despite the fact that a low mass of the external potential (Mext <  1.0 ×  Mstars) may promote the formation of wider binaries, these systems tend to be short-lived due to the higher velocities of all the stars. This figure is only intended to show the distribution of the semi-major axis and not the total number of binaries that formed.

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