Time evolution of the difference between the velocity dispersion of the high-mass stars (‘H’, 0.8 ≤ m/M_⊙ ≤ 1.0) and that of the low-mass stars (‘L’, 0.1 ≤ m/M_⊙ ≤ 0.2). The velocity dispersion is scaled by $\widehat{\sigma }=r_{\mathrm{h},0}^{-1/2}$. The rows show the difference in the total σ (top), its radial component (middle), and its tangential component (bottom). The columns are separated by models (as labelled on top). Each plot has three lines which represent three outside regions of the clusters, delimited by the listed Lagrangian radii.