Evolution of scale radii: Evolution of the GC+DM system tidal radius (r_t, blue) and of the half-mass radius of the bound dark matter particles (r_1/2, •, black), for each simulated cluster. We observe that clusters who lost most of their dark matter mini-halo (i.e. GC1 and GC2) presented r_t >  r_1/2, • at some point of their orbital evolution, similarly to the relation for sub-halo disruption from Hayashi et al. (2003).