Evolution of the 0.2, 0.5, and 0.8 Lagrangian radius of the tidal tail for number of stars (solid lines). Left and right panels represent the lower (M_cl(0) = 1400 M_⊙) and higher mass (M_cl(0) = 4400 M_⊙) clusters, respectively. The half-number radius (i.e. the 0.5 Lagrangian radius) is indicated by the thick solid lines. The semi-analytical half-number radius calculated by Eq. (20) in Paper I and scaled to the value of (see Table 1) for the corresponding model is shown by the dotted lines. The semi-analytical prediction is very good for the models dominated by tail I (models C03G13 and C10G13; red lines), but it is rather poor for the models with a non-negligible population of tail II stars (models C03G23, C10G23, C03GA, and C10GA).