Table 5
Dynamical history of highly mutually inclined systems. The first column shows all the possible outcomes.
| Dynamical history | # | 1.4 × 106 yr | 1.0 × 108 yr |
|
|
|||
| Ejection/collision | 2 | 38% | 45% |
| Ejection/collision + MMR | 2 | 20% | 16% |
| 3-B reso + ejection/collision | 2 | 5% | 17% |
|
|
|||
| Orb. instability | 3 | 9% | 8% |
| Orb. instability + 3-B reso | 3 | 17% | 8% |
| 3-B reso | 3 | 10% | 6% |
| 3-B reso + orb. instability | 3 | 1% | 0% |
Notes. For two-planet systems, ejection/collision induced by planet-planet scattering, ejection or collision followed by an inclination-type resonance and ejection/collision after a three-body resonance are the possible scenarios. For three-planet systems, orbital re-arrangement followed or not by a three-body resonance, three-body resonance and orbital re-arrangement after capture in three-body resonance are the four scenarios. The second column gives the number of planets at the end of simulation. The last two columns give the percentages of each scenario for different integration times.
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