Table 1.
Parameters of observed exoplanets (http://exoplanet.eu/) that we used as input parameters in the model and the resulting H,He fraction estimates for standard core-envelope models and for planets formed with polluted envelopes and rain out their silicates afterwards.
| Mass | Radius | Period | Age | H,He | H,He | |
|---|---|---|---|---|---|---|
| (M⊕) | (R⊕) | (day) | (Gyr) | standard | w/ rainout | |
| Kepler-36 c | 7.13 | 3.6 | 16.2 | 6.9±0.372 | 7.8% | 6% |
| Kepler-11 e | 7.95 | 4.1 | 32 |
 |
15% | 11% |
| TOI-1136 d | 7.95 | 4.53 | 12.5 | 0.7±0.1 | 13% | 6.5% |
| TOI-1136 f | 8.3 | 3.8 | 26.3 | 0.7±0.1 | 9% | 4.5% |
| TOI-1422 b | 8.9 | 3.88 | 13 |
 |
10% | 6% |
| KOI-142 b | 9.54 | 3.37 | 10.9 |
 |
7% | 4% |
| K2-314 d | 10.2 | 3.86 | 35.7 | 9±0.6 | 13% | 10% |
| K2-19 c | 10.8 | 4.76 | 11.9 | 8+ | 20% | 14% |
| Kepler-79 b | 10.9 | 3.4 | 13.5 |
 |
6.6% | 4.5% |
| Kepler-30 b | 11.4 | 3.82 | 29.3 | 2±0.8 | 11% | 6% |
Notes. The selected planets are all the exoplanets with masses 7–12 M⊕, radii above 3.3 R⊕, and estimates for stellar age (marked in green in Fig. 5). Error bars were omitted from all observation values and we calculate each model for a single set of values.
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