Outwards motion of the corona stars with respect to the pair of star clusters’ centre of mass. Smoothed magnitudes V_r of residual line-of-sight velocities of receding (approaching) stars from Gaia DR3 are shown by red (blue) lines. The mean residual tangential velocities in the picture plane V_t are shown by the green line. The grey line shows the mean tangential components of the runaway velocities obtained in N-body simulations for the Dehnen γ = 0 initial stellar profile with SFE = 0.05 after 50 Myr of evolution (Shukirgaliyev et al. 2021), where the shadow represents the uncertainty.