Table 2
Summary of our simulation results for the different models.
| Ice line evolution | Planet migration | Water content of inner planets (r < 0.3 AU) | Figure |
|---|---|---|---|
| No | No | Only rocky by construction, no water rich planets | Fig. 2 |
| No | Yes | Mostly rocky, some water rich planets originating from beyond  |
Fig. 3 |
| Yes | No | Only rocky by construction, no water rich planets | Fig. 4 |
| Yes | Yes | Only rocky planets, water rich planets trapped outside of 0.7 AU | Fig. 5 |
| Yes | Only inwards | Rocky and icy planets with composition gradient depending on r0 | Fig. 6 |
| Yes | Yes | Fast growth allows rocky interior planets, no inner water rich planets | Fig. 8 (top) |
| Yes | Yes | Slow growth allows rocky interior planets, no inner water rich planets | Fig. 8 (bottom) |
Notes.Observational predictions imply that close in super-Earth planets (r < 0.3 AU) are predominately rocky, but that there are also icy super Earths (Owen & Wu 2013; Lopez & Fortney 2014; Fulton & Petigura 2018; Jin & Mordasini 2018; Van Eylen et al. 2018b). Only the models shown in Figs. 3 and 6 allow for rocky and ice rich inner planets within the same framework, but the water ice line of the model presented inFig. 3 does not evolve in time, which we deem unrealistic.
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