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Table 2
Distribution of trapping in a 1:1 resonance, collisions, crossings, and trappings that are MMRs or gap trappings due to the equality between the gas disk and pebble angular velocities.
| Mass ratio | Collision radius | Co-orbitals | Collisions | Crossings | Trappings |
|
|
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| μ2 = 10-4 | 0.005 RHill | − | 40% | 58% | 2% |
| (b = 0.1) | 0.05 RHill | − | 42% | 56% | 2% |
| μ2 = 3 × 10-4 | 0.005 RHill | − | 39% | 1% | 60% |
| (b = 0.25) | 0.05 RHill | − | 40% | 1% | 59% |
| μ2 = 3 × 10-4 | 0.005 RHill | − | 22% | 1% | 77% |
| (b = 0.3) | 0.05 RHill | − | 23% | 1% | 76% |
| μ2 = 6 × 10-4 | 0.005 RHill | − | 6% | 1% | 93% |
| (b = 0.5) | 0.05 RHill | − | 6% | 1% | 93% |
| μ2 = 6 × 10-4 | 0.005 RHill | − | <1% | <1% | 99% |
| (b = 0.6) | 0.05 RHill | − | 1% | <1% | 98% |
| μ2 = 10-3 | 0.005 RHill | − | <1% | <1% | 99% |
| (b = 0.9) | 0.05 RHill | − | <1% | <1% | 99% |
| μ2 = 10-3 | 0.005 RHill | − | <1% | <1% | 99% |
| (b = 0.99) | 0.05 RHill | − | <1% | <1% | 99% |
Notes.The range of the planet eccentricity is the same as the one in Table 1.
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