Table F.1
Statistics of the results from our simulations of compact-system instability
| Statistics of compact systems’ instability | ||||||||
| N0 | T1 | T2 | T3 | T4 | T5 | T6 | Average | |
| Total systems | 90 | 23 | 90 | 90 | 90 | 90 | 12 | - |
| N. unstable | 21 | 14 | 19 | 17 | 19 | 13 | 6 | - |
| N. unstable (%) | 23 | 61 | 21 | 19 | 21 | 14 | 50 | 29 ± 17 |
| Pathway of formation of the simulated metal-rich planets | ||||||||
| N0 | T1 | T2 | T3 | T4 | T5 | T6 | Average | |
| Target disruption (%) | 0.5 | 0.5 | 3.2 | 1.8 | 0.4 | 0.0 | 0.1 | 1 ± 1 |
| Hit-and-run (%) | 99.5 | 99.5 | 96.8 | 98.2 | 99.6 | 100.0 | 99.9 | 99 ± 1 |
| Occurrence rate (%) of the simulated metal-rich planets | ||||||||
| N0 | T1 | T2 | T3 | T4 | T5 | T6 | Average | |
| ηMR | 1.6 | 0.8 | 0.8 | 2.7 | 1.9 | 1.8 | 1.6 | 1.6 ± 0.6 |
| ηMR (R <1 R⊕) | 17.4 | 8.9 | 7.4 | 19.4 | 18.2 | 42.9 | 30.3 | 21 ± 12 |
| ηMR | 0.4 | 0.1 | 0.1 | 1.3 | 0.4 | 0.3 | 0.6 | 0.5 ± 0.5 |
| Radius R(R⊕) of the simulated metal-rich planets | ||||||||
| N0 | T1 | T2 | T3 | T4 | T5 | T6 | Average | |
| Minimum | 0.2 | 0.2 | 0.2 | 0.2 | 0.2 | 0.2 | 0.4 | 0.2 ± 0.1 |
| Mean value | 0.8 | 0.8 | 0.7 | 0.9 | 0.8 | 0.9 | 1.2 | 0.9 ± 0.2 |
| 68th percentile | 1.0 | 1.0 | 0.9 | 0.9 | 1.0 | 1.0 | 1.3 | 1.0 ± 0.1 |
| 95th percentile | 1.2 | 1.3 | 1.0 | 1.6 | 1.2 | 1.3 | 1.6 | 1.3 ± 0.2 |
| 99.7th percentile | 1.5 | 1.6 | 1.1 | 2.2 | 1.4 | 1.5 | 1.7 | 1.6 ± 0.3 |
| Maximum | 1.7 | 1.7 | 1.1 | 2.2 | 1.5 | 1.5 | 1.8 | 1.6 ± 0.3 |
| Mass M (M⊕) of the simulated metal-rich planets | ||||||||
| N0 | T1 | T2 | T3 | T4 | T5 | T6 | Average | |
| Minimum | 0.006 | 0.006 | 0.006 | 0.004 | 0.006 | 0.01 | 0.07 | 0.02 ± 0.02 |
| Mean value | 1.0 | 1.0 | 0.6 | 1.4 | 1.0 | 1.0 | 2.9 | 1.3 ± 0.7 |
| 68th percentile | 1.3 | 1.1 | 1.0 | 1.1 | 1.4 | 1.4 | 3.5 | 1.6 ± 0.8 |
| 95th percentile | 2.5 | 2.9 | 1.3 | 6.4 | 2.4 | 2.7 | 6.1 | 4 ± 2 |
| 99.7 th percentile | 5.4 | 7.0 | 1.5 | 23.0 | 4.9 | 4.9 | 7.6 | 8 ± 7 |
| Maximum | 8.0 | 8.0 | 1.9 | 23.5 | 5.2 | 5.2 | 11.5 | 9 ± 7 |
Notes. Statistics of metal-rich planets formed during an orbital instability in the nominal scenario (N0) and its variations (T1-T6). The statistics in every column are computed across 109 000 simulations (1000 simulations for each of the 109 unstable systems). The uncertainties in the rightmost column correspond to one standard deviation.
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