Table 1
Input parameters for our calculations.
| Planet | Mass (M⊕) | Radius (R⊕) |  (kg m−3) |
Teff (K) | Orbital period (day) | Eccentricity |
|---|---|---|---|---|---|---|
| b | 0.79 ± 0.27 | 1.086 ± 0.035 |  |
400 | 1.5108739 ± 0.0000075 | 0.019 ± 0.008 |
| c | 1.63 ± 0.63 | 1.056 ± 0.035 |  |
342 | 2.421818 ± 0.000015 | 0.014 ± 0.005 |
| d | 0.33 ± 0.15 | 0.772 ± 0.030 |  |
288 | 4.04982 ± 0.00017 |  |
| e |  |
0.918 ± 0.039 |  |
251 | 6.099570 ± 0.000091 | 0.007 ± 0.003 |
| f |  |
1.045 ± 0.038 |  |
219 | 9.20648 ± 0.00053 | 0.011 ± 0.003 |
| g | 0.566 ± 0.036 | 1.127 ± 0.041 |  |
199 | 12.35281 ± 0.00044 | 0.003 ± 0.002 |
| h |  |
0.7150 ± 0.047 |  |
167 | 18.76626 ± 0.00068 | 0.086 ± 0.032 |
Notes. Mass, radius, effective temperature, orbital period and eccentricity data are from Wang et al. (2017). We have calculated mean densities and uncertainties on density based on the best-fit values and extrema of masses and radii. (a) Minimum values of mass and density reported here permit the presence of a small, low-density rock core, which is plausible based on geochemical arguments. (b) We set the mean and the minimum density values to correspond to an ice planet with a small, low-density rock core.
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