From Fig 10, it can be seen that relative to the original values, the eccentricities of the low masses (Bins 0 \(\rightarrow\) 100) only increase by 5.59%, while the inclinations only increase by 4.26%. For the breakpoint masses (around Bin 118), the eccentricities and inclination both increase by 9%, while for the high masses (Bins 121 \(\rightarrow\) 127), their eccentricities increase by roughly 7% and their inclinations increase by roughly 7.5%.

These differences are nearly negligible considering how the initial conditions \((e_0^\prime, i_0^\prime)\) were 1000% of the original. This shows that the effects of Viscous Stirring and Dynamical Friction are weak at these higher eccentricities and inclinations. It also implies that for any of the masses to reach \((e, i)\approx0.02\) within the age of the Solar System, they would need initial conditions \((e_0^\prime, i_0^\prime)\) to be on the same order, with a near negligible evolution rate.