Fig. 3.

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Velocity anisotropy: Evolution of the orbital radius (i.e. rorbit, upper plots) and of the outer velocity anisotropy (i.e. β∞, lower plots), for the five simulated globular clusters. The clusters originally embedded in a dark matter mini-halo are depicted in solid green, and those without it are displayed in solid red. For β∞, we display the running mean over the five closest snapshots (time-wise), for better visualisation, which explains why the initial β∞ values seem to be different for the two scenarios. We observe typically lower rorbit and more radial (i.e. higher) β∞ for clusters with a dark matter mini-halo.
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