Table 3
General characteristics of the most distinctive planets formed in the S1, S2, and S3 simulations using a disk of 0.125 M⊕.
| Simulation | Planet | a (AU) | e | i (°) | M (M⊕) | TLGI (Myr) | W (%) |
|
|
|||||||
| S1 | Innermost planet | 0.48 | 0.11 | 6.88 | 0.97 | 6.71 | 7.4 |
| HZ planet | 0.93 | 0.06 | 3.36 | 3.16 | 25.6 | 9.1 | |
| Most massive planet | 1.97 | 0.01 | 1.3 | 13.4 | 44.03 | 43.19 | |
| S2 | Innermost planet | 0.63 | 0.17 | 4.69 | 1.56 | 7.13 | 6.35 |
| HZ planet | 1.16 | 0.08 | 2.69 | 4.74 | 6.48 | 44.2 | |
| Most massive planet | 2.54 | 0.04 | 1.69 | 10.05 | 16.2 | 42.4 | |
| S3 | Innermost planet | 0.78 | 0.13 | 3.44 | 2.63 | 28.83 | 4.05 |
| HZ planet | 1.15 | 0.11 | 3.32 | 1.89 | 0.59 | 8.31 | |
| Most massive planet | 2.02 | 0.04 | 1.44 | 12.66 | 6.92 | 49.1 | |
Notes. a is the semimajor axis of the resulting planets in AU, e the eccentricity, i the inclination in degrees, M the final mass in M⊕, TLGI the timescale in Myr associated with the last giant impact produced by an embryo, and W the percentage of water by mass after 200 Myr of evolution.
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