Table 1
Exploration of hydrodynamical simulations to form resonant chains with four or five planets.
| h | Name | Planet order | Resonant chain |
|---|---|---|---|
| 4 Planets | |||
| 0.05 | N4 | J-S-U-N | (2:1,3:2,4:3) |
| 0.05 | Nbis4 | J-S-N-U | (2:1,2:1,4:3)(*) |
| 0.035 | C4 | J-S-U-N | (2:1, 3:2, 5:4) |
| 5 Planets | |||
| 0.05 | J-S-U-N-U | Unstable | |
| 0.05 | J-S-U-N-U(†) | Unstable | |
| 0.05 | J-S-U-N-P9 | Unstable | |
| 0.05 | J-S-N-U-U | Unstable | |
| 0.05 | Nbis5 | J-S-N-U-U(†) | (2:1, 2:1, 4:3, 5:4) |
| 0.035 | J-S-U-N-U | Unstable | |
| 0.035 | J-S-U-N-U(†) | Unstable | |
| 0.035 | C5 | J-S-U-N-P9 | (2:1, 3:2, 5:4, 4:3) |
| 0.05 | J-S-P9-U-N | Unstable | |
| 0.035 | J-S-P9-N-U | Unstable | |
Notes. This table shows the cases presented in Sects. 2.2.1 and 2.2.2, and all cases that did not manage to form a stable resonant chain, to emphasize the difficulty of forming long resonant chains in low-viscosity discs. Column 1 – disc aspect ratio h. Column 2 – simulation name if it resulted in a stable configuration. Column 3 – radial order of the planets in the disc. Column 4 – final resonant chain at the end of the simulation, if stable. (†) Different introduction time with respect to the above line. (*)Stable after having ejected an ice giant.
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