Regolith Capture around Chariklo.
All simulations below have 6 degrees of Gravitational Harmonics (unless mentioned otherwise).
Here regolith is ejected with a landslide-like ejection with a random variance of 30º.
The regolith have an initial ejection velocity in the range of 0.2 - 0.5 v_escape.
X vs Y on the left, and a vs e on the right.
The regolith below have an initial ejection velocity in the range of 0.1 - 0.3 v_escape.
X vs Y on the left, and a vs e on the right.
Regolith capture with a new ejection into a previously captured disk.
The disk is taken from the 0.2-0.5 v_escape simulation at t = 50 rotations.
Here the new regolith is ejected radially with a random variance of 30º.
The new regolith have an initial ejection velocity in the range of 0.1 - 0.3 v_escape.
X vs Y on the left, and a vs e on the right.
Stability of Initial Trajectories.
Here I plot the orbits of initial ejection trajectories of regolith around Chariklo.
We see a loosely defined curve that we call the "Pericenter Curve/Tisserand Tail". It marks
stable (below) and unstable (above) orbits around a perfectly spherical body.
0º is radial ejection, while 90º is tangential (landslide-like) ejection.
Gravitational Harmonics effect on a vs e.
We use 6 degrees of Gravitational Harmonics here.
One can see the excitation of orbits caused by the gravitational harmonics and the "Pericenter Curve/Tisserand Tail".
Particles above this curve are in unstable orbits around a perffectly spherical body.
The ellipsoidal shape of Chariklo cause angular momentum exchange and the excitation of orbits.
t = 2 rotations above, t = 10 rotations below.
Here I show the effect of J2 and C22 of Chariklo.
This is our recreation of Winter et al (2023).
Here I show the effect of J2 and C22 on test particles on circular orbits around Chariklo.
These simulations show that Gravitational harmonics will excite disks in ring-like structures.
t = 2 days above, t = 10000 days below.