Orbital crossing time (t_cross) of each planet pair is plotted as a function of the orbital separation in the mutual Hill radius (Δ). Left panels: results in the massive series (models Ms1Σ100b10, Ms3Σ30b10, and Ms5Σ10b10), and right: those in the less-massive series (models Ms0Σ100b10, Ms2Σ30b10, and Ms4Σ10b10), respectively. Three dotted lines are the orbital crossing time with e = 0 planets (left one), 0.5e_esc,M1 planets (middle one), and e_esc,M1 planets (right one) estimated by Eq. (A.1).