deletions | additions       diff --git a/Fig_5_shows_the_evolution__.tex b/Fig_5_shows_the_evolution__.tex  index b5abde5..69fbdea 100644  --- a/Fig_5_shows_the_evolution__.tex  +++ b/Fig_5_shows_the_evolution__.tex 
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Looking at Fig 6, after the masses redistribute orbital energy during the first 10Myrs, they all appear to follow a stable logarithmic increase. If we assume the increase to remain roughly linear on a log scale, it can be estimated that the masses would only reach $(e, i)\approx0.02$ after a period of $10^8$Myrs.  This shows that for the initial conditions used, self-stirring effects alone are unable to reproduce the  observed values orbital properties of CCKBOs  within the age of the Solar System.