Table 1
Initial conditions of our simulations.
| Radial | Mutual | tstart | ||
|---|---|---|---|---|
| distribution | separation | |||
| Model | I | 0.7 to ~20 AU | 0.25 AU (~5−100 Rhm) | 0.5 and 3 Myr |
| II | 0.7 to ~60 AU | ~0.01−3 AU (~10−30 Rhm) | 0.5 and 3 Myr | |
| III | 0.2 (or 0.3) to ~2 AU | 0.025 AU (~15−55 Rhm) | 0.5 and 3 Myr | |
Notes. From left to right,columns mark the simulation model, the region where planetary seeds are initially distributed in the disk, their initial mutual radial separation, and the disk age at the start of the simulation. The mutual separation is also given in units of mutual hill radii, 
, where m1 and m2 are the masses and a1 and a2 are the semi-major axes of any two adjacent planetary embryos.
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