Table A.3
Physical characteristics of the exoplanets we used in the study of some real cases.
| Exoplanet | Mass | Radius | Semi-major | HZ | Mean orbital | Rotation | Tidally | Magnetic |
|---|---|---|---|---|---|---|---|---|
| (in M⊕) | (in R⊕) | axis (AU) | eccentricity | (days) | locked | moment | ||
| Barnard’s b (a) | 3.23 | 1.60 (e) | 0.404 | COLD | 0.295 | – | N | 2.47 |
| GJ 2232 b (b) | 2.02 | 1.22 (e) | 0.033 | INNER EDGE | 0.230 | 3.576 | Y | 0.70 |
| GJ 2232 c (b) | 2.31 | 1.31 (e) | 0.126 | COLD | 0.215 | 40.54 | Y | 0.04 |
| GJ 581 e (b) | 1.94 | 1.20 (e) | 0.028 | HOT | 0.320 | 2.100 | Y | 1.02 |
| K2-3 d (b) | 11.09 | 1.48 | 0.209 | INNER EDGE | 0.045 | 44.56 | Y | 2.2 |
| Kepler-1185 b (b) | 2.29 (e) | 1.31 | 0.428 | INNER EDGE | 0 | – | N | 0.76 |
| Kepler-1229 b (b) | 2.49 (e) | 1.37 | 0.311 | GREEN | 0 | – | N | 0.19 |
| Kepler-1649 b (b) | 1.22 (e) | 1.06 | 0.050 | HOT | 0 | 8.689 | Y | 0.22 |
| Kepler-186 f (b) | 1.34 (e) | 1.09 | 0.392 | GRENN | 0 | – | N | 1.3 |
| Kepler-22 b (b) | 6.00 (e) | 2.30 | 0.848 | GREEN | 0 | – | N | 0.77 |
| Kepler-442 b (b) | 2.33 (e) | 1.32 | 0.386 | GREEN | 0.04 | – | N | 8.4 |
| Kepler-62 e (b) | 35.91 (e) | 1.58 | 0.426 | INNER EDGE | 0 | – | N | 92.0 |
| Kepler-62 f (b) | 35.96 (e) | 1.38 | 0.718 | GREEN | 0 | – | N | 68.0 |
| Proxima Cen. b (c) | 1.27 | 1.07 (e) | 0.048 | GREEN | 0.175 | 11.186 | Y | 0.19 |
| Ross 128 b (b) | 1.40 | 1.10 (e) | 0.050 | HOT | 0.116 | 9.866 | Y | 0.23 |
| Teegarden’s b (b) | 1.05 | 1.01 (e) | 0.025 | INNER EDGE | 0.08 | 4.910 | Y | 0.30 |
| Teegarden’s c (b) | 1.11 | 1.03 (e) | 0.044 | GREEN | 0.08 | 11.409 | Y | 0.16 |
| Trappist-1 c (d) | 1.38 | 1.06 | 0.015 | HOT | 0.042 | 2.422 | Y | 1.10 |
| Trappist-1 d (d) | 0.41 | 0.77 | 0.021 | HOT | 0.035 | 4.050 | Y | 0.15 |
| Trappist-1 e (d) | 0.64 | 0.90 | 0.028 | GREEN | 0.043 | 6.100 | Y | 0.10 |
| Trappist-1 g (d) | 1.34 | 1.13 | 0.045 | GREEN | 0.031 | 12.353 | Y | 0.06 |
| Trappist-1 h (d) | 0.37 (e) | 0.76 | 0.066 | OUTER EDGE | 0.0 | 20.000 | Y | 0.03 |
| Wolf 1061 b (b) | 1.91 | 1.20 (e) | 0.036 | HOT | 0.165 | 4.887 | Y | 0.52 |
| YZ Cet b (b) | 0.76 | 0.93 (e) | 0.016 | HOT | 0.060 | 1.969 | Y | 0.46 |
| YZ Cet c (b) | 0.99 | 1.0 (e) | 0.021 | HOT | 0.055 | 3.060 | Y | 0.46 |
| YZ Cet d (b) | 1.14 | 1.04 (e) | 0.028 | HOT | 0.129 | 4.656 | Y | 0.33 |
Notes. When planetary mass and radius were unknown, we estimated them based on results of Chen & Kipping (2017). The rotational period of tidally locked exoplanets was obtained using the most likely spin-orbit resonance according to Dobrovolskis (2007). The rest of the columns are described in the text.
References. (a) Ribas et al. (2018), (b) Esitmated using Chen & Kipping (2017), (c) http://exoplanet.eu/catalog/ (d) Anglada-Escudé et al. (2016), (e)Gillon et al. (2017).
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