Table B.1
Summary of differences between additional simulations discussed in Appendix B and the nominal simulation.
| Simulation | Scold | S1 | S2 | S3 | S4 |
|---|---|---|---|---|---|
| Mass doubling time tacc(a) | N/A | 0.5 Myr | 0.5 Myr | – | – |
| Opacity law | – | – | uniform (b) | – | – |
| Planet’s orbital distance rp(a) | – | – | – | 85 au | – |
| Inner radial boundary (a) | – | – | – | 28 au | – |
| Outer radial boundary (a) | – | – | – | 180 au | – |
| Planet mass Mp(a) | – | – | – | – | 20 M⊕ |
| Smoothing length rsm(a) | – | – | – | – | 0.5 RH |
| No. of orbits to introduce Mp(a) | – | – | – | – | 5 |
| No. of simulated orbits (a) | – | – | – | – | 25 |
| Putative gap amplitude Ag | N/A | N/A | N/A | N/A | 5 |
| Putative gap centre rg | N/A | N/A | N/A | N/A | 80 au |
| Putative gap width wg | N/A | N/A | N/A | N/A | 15 au |
Notes. Dashes imply that a parameter keeps the nominal value. When a parameter is not applicable (not used in the model), we write ‘N/A’. (a) Applies to the final simulation stage with an embedded planet. The time span of the hydrodynamic relaxation stage is 800 orbits for simulation S4 and 200 orbits otherwise. (b) When using the primitive uniform opacity model, we assume that the Planck and Rosseland opacities are identical and equal to 1 cm2 g−1 while the opacity to stellar irradiation amounts to 3 cm2 g−1 (all values being expressed per gram of gas).
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