It can be seen from Fig 8, using the same notation from Fig 5, that the low masses do not undergo the same rapidly evolving early stage as in Fig 5, but do later follow a similar logarithmic increase. The breakpoint masses barely evolve from their initial eccentricity and inclination, seemingly appearing stable, though at the later stages a very slow increase can be noticed. The high masses evolve towards a more circular and planar orbit, despite the initial conditions already being relatively circular and planar compared to the observed conditions, after which they quickly enter a stable orbital state which slowly increases logarithmically.

The early stages of evolution from Fig 8 are very different from the original’s Fig 5, which can be examined in more detail with their respective log scale plots Fig 9 and Fig 6. As previous mentioned for Fig 6, the early stage involving the orbital energy transfer due to Dynamical Friction is measurable after a few decades and lasts until roughly 10Myrs, after which the masses stabilize and follow a logarithmic rate of change due to Viscous Stirring. In comparison for Fig 9, the first measurable changes only occur after 1Myr and the effects of Dynamical Friction continue to evolve the system until roughly 400Myrs, at which point the Dynamical Friction effects diminish and Viscous Stirring slowly becomes the dominant driving force of the evolution.

This comparison implies that at eccentricities and inclinations on the order of 0.001, the effects of Viscous Stirring and Dynamical Friction are significantly diminished, resulting in slow evolution rates. This is supported by examining the difference between the values of \((e^\prime, i^\prime)\) and \((e, i)\) at 4000Myrs.