Table 1
Characteristics of the planets considered in this article.
| Planet | Mass (kg) | Radius (km) | Water mass fraction (%) | Fe/Si (% wrt ⊕) |
|---|---|---|---|---|
| 0.5 M⊕ planet | 2.98 × 1024 | 5376 | 0 | 50 |
| 5214 | 100 | |||
| 5 088 | 150 | |||
| Earth-like | 5.95 × 1024 | 6573 | 0 | 50 |
| 6 364 | 100 | |||
| 6217 | 150 | |||
| 5 M⊕ super Earth | 2.98 × 1025 | 10 246 | 0 | 50 |
| 9908 | 100 | |||
| 9670 | 150 | |||
| 10 M⊕ super Earth | 5.95 × 1025 | 12 216 | 0 | 50 |
| 11 823 | 100 | |||
| 11 547 | 150 | |||
| TRAPPIST-1e | 4.60 × 1024 | 5800 | 0 | 138 |
| 6002 | 5 | 150 | ||
| TRAPPIST-1f | 5.56 × 1024 | 6670 | 11 | 100 |
| 6666 | 14.5 | 150 | ||
| TRAPPIST-1g | 6.83 × 1024 | 7314 | 19 | 100 |
| 7308 | 22.5 | 150 | ||
| TRAPPIST-1h | 1.97 × 1024 | 4924 | 10 | 100 |
| 4930 | 13.5 | 150 | ||
| Venus | 4.85 × 1024 | 6152 | 0 | ~100 |
Notes. As we are not studying the impact of Earth’s ocean, we are not treating Earth in itself but, rather, an Earth-like planet of same mass and radius. However, we are treating Venus with as much details as we can based on the literature dedicated to this planet (following Dumoulin et al. 2017, see Sect. 2.3.2).
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