(Adjust collisional rates for the outer MB, use randomly assigned YORP evolution of Gaussian spheres.)
(Lighter hot disc?)
http://www.mplayerhq.hu
).
Jupiter was started at 5.202 AU,
50 ME cold planetesimal disc
j21_pdisc_50ME_cold_I00j_aet.avi
j21_pdisc_50ME_cold_I00j_ait.avi
j21_pdisc_50ME_cold_I00j_xyt.avi
j21_pdisc_50ME_cold_I00j_xzt.avi
2DO: 30 ME cold planetesimal disc
2DO: 30 ME hot planetesimal disc
j32_pdisc_50ME_cold_I00j_aet.avi
j32_pdisc_50ME_cold_I00j_ait.avi
2DO: 30 ME cold planetesimal disc
2DO: 30 ME hot planetesimal disc
2DO: integrate hundreds of Thule and 2001 QG207 clones
2DO: 30 ME cold planetesimal disc
2DO: 30 ME hot planetesimal disc
Jupiter was started at 5.45 AU,
50 ME cold planetesimal disc
j21_pdisc_50ME_cold_I00_aet.avi
j21_pdisc_50ME_cold_I00_ait.avi
j21_pdisc_50ME_cold_I00_xyt.avi
j21_pdisc_50ME_cold_I00_xzt.avi
j43_pdisc_50ME_cold_I00_aet.avi
j43_pdisc_50ME_cold_I00_ait.avi
j43_pdisc_50ME_cold_I00_xyt.avi
j43_pdisc_50ME_cold_I00_xzt.avi
2DO:
2DO: different configurations of planets, planetesimal disc masses, ...
2DO: r21-impye run
2DO: a longer run with collisions and YORP included
Both stable and unstable in the J2/1 are included here.
2DO: already calculated, have to include collisions and YORP for the smalles bodies...
2DO: is still running...
variable | number of integrations | notes |
inicond of planets | >3 sets | aJ = 5.45 AU |
Mdisc | 2-3 sets | 30, 35, 40 M_E |
hot/cold disc | >2 sets | e, sin i = 10-3 or 0.05 |
number of PLs | >2 sets | 3500, 5000, 7500 |
number of TPs | 1 or more | |
sigma(r) | 1 trial | r-1.5 or even steeper falloff |
integration accuracy | 1 trial | |
SyMBA vs Mercury | 1 trial | |
self gravity | 1 trial | |
beginning and the end of the disc | 1 trial |
We provide a complete update of resonant populations based on recent orbital catalogues. There are approximately 150 long-lived objects in the J2/1 resonance, ~1000 in the J3/2 and only a few objects in J4/3. We classify them according to their dynamical lifetimes, as inferred from N-body simulations spanning ~4 Gyr, and we present available physical properties and size-frequency distributions for the respective sub-groups.
We compute long-term orbital evolution of resonant bodies driven by slow chaotic diffusion, the Yarkovsky effect and collisions. We also test the stability of the resonant orbits under the influence of various mutual resonances between Jupiter and Saturn (1:2, 3:7, 4:9, 2:5), which were possibly encountered during the planetary migration period.
Miroslav Broz (mira@sirrah.troja.mff.cuni.cz), Aug 4th 2006