this is for holding javascript data
Rory Hopkins edited Fig_5_shows_the_evolution__.tex
about 8 years ago
Commit id: ec86e256c42006cb5a9c3a78783a4ac928fe6e00
deletions | additions
diff --git a/Fig_5_shows_the_evolution__.tex b/Fig_5_shows_the_evolution__.tex
index 0402c41..ed872ef 100644
--- a/Fig_5_shows_the_evolution__.tex
+++ b/Fig_5_shows_the_evolution__.tex
...
While these values are expectedly low, they are too low by more than 1 order of magnitude of the observed values of $(e, i)\approx0.02$, including the low masses which reach the highest values.
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 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 $10^8$Myrs.
This shows that for the initial conditions used, self-stirring effects alone are unable reproduce observed values within the age of the Solar System.