Table 4
Retrieved core mass fraction (CMF) and water mass fraction (WMF) of planets in the multi-planetary systems K2-138, TOI-178, Kepler-11, Kepler-102, and Kepler-80, with our interior-atmosphere model.
| System | Planet | CMF | WMF | dobs-ret | ΔMH2 (Μ⊕) | ΔMH2O (Μ⊕) | ΔMXUV (Μ⊕) |
|---|---|---|---|---|---|---|---|
| b | 0.27 ± 0.02 |  |
1.5 σ | 0.132 | <0.01 | 0.40 | |
| c | 0.23 ± 0.02 | 0.13 ± 0.04 | <1 σ | <0.01 | <0.01 | <0.01 | |
| K2-138 | d | 0.22 ± 0.03 | 0.17 ± 0.05 | <1 σ | <0.01 | <0.01 | <0.01 |
| e | 0.11 ± 0.02 | 0.57 ± 0.08 | <1 σ | <0.01 | <0.01 | <0.01 | |
| f | 0.11 ± 0.02 | 0.60 ± 0.07 | <1 σ | <0.01 | <0.01 | <0.01 | |
| g | 0.12 ± 0.05 | 0.55 ± 0.18 | 1.3 σ | <0.01 | <0.01 | <0.01 | |
| b | 0.21 ± 0.30 | 0 | <1 σ | 0.83 | <0.01 | 0.45 | |
| c | 0.30 ± 0.02 |  |
<1 σ | <0.01 | <0.01 | 0.21 | |
| TOI-178 | d | 0.10 ± 0.01 | 0.69 ± 0.05 | 1.3 σ | 0.16 | <0.01 | 0.48 |
| e | 0.18 ± 0.02 | 0.40 ± 0.06 | <1 σ | <0.01 | <0.01 | 0.13 | |
| f | 0.22 ± 0.03 | 0.28 ± 0.10 | <1 σ | <0.01 | <0.01 | 0.04 | |
| g | 0.10 ± 0.01 | 0.58 ± 0.16 | 3.0 σ | <0.01 | <0.01 | 0.11 | |
| b | 0.20 ± 0.04 | 0.27 ± 0.10 | <1 σ | <0.01 | <0.01 | 0.10 | |
| c | 0.18 ± 0.01 | 0.33 ± 0.04 | 1.7 σ | <0.01 | <0.01 | 0.10 | |
| Kepler-11 | d | 0.10 ± 0.02 | 0.65 ± 0.05 | 2.4 σ | <0.01 | <0.01 | 0.13 |
| e | 0.12 ± 0.01 | 0.55 ± 0.04 | 4.4 σ | <0.01 | <0.01 | 0.14 | |
| f | 0.14 ± 0.06 | 0.47 ± 0.10 | 1.9 σ | 0.56 | <0.01 | 0.06 | |
| b |  |
0 | <1 σ | 0.13 | <0.01 | 0.03 | |
| c |  |
0 | <1 σ | 0.10 | <0.01 | 0.03 | |
| Kepler-102 | d | 0.80 ± 0.14 | 0 | <1 σ | <0.01 | <0.01 | 0.03 |
| e | 0.22 ± 0.02 | 0.17 ± 0.07 | <1 σ | 0.01 | <0.01 | 0.03 | |
| f | 0.27 ± 0.09 | 0.04 ± 0.04 | <1 σ | 0.02 | <0.01 | 0.01 | |
| d |  |
0 | <1 σ | <0.01 | <0.01 | 0.35 | |
| e | 0.43 ± 0.18 | 0 | <1 σ | <0.01 | <0.01 | 0.29 | |
| Kepler-80 | b | 0.13 ± 0.02 | 0.58 ± 0.07 | <1 σ | <0.01 | <0.01 | 0.11 |
| c | 0.09 ± 0.01 | 0.70 ± 0.04 | <1 σ | <0.01 | <0.01 | 0.13 | |
| g | 0.31 ± 0.02 | <1.5 × 10−3 | <1 σ | 140 | 3.23 | 0.60 | |
Notes. A low dobs-ret indicates that the assumption of a water-dominated atmosphere is adequate for a particular planet (see text). We note that ΔMH2, ΔMH2O, and ΔMXUV correspond to the maximum estimate of atmospheric escape mass loss due to H2, water Jeans escape, and XUV photoevaporation, respectively.
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