Table 10
Comparison of Gl 486 b and Solar System telluric planets’ interior and atmospheric parameters.
| Planet | Model(a) | log mupper/Mp | mmantle/Mp | mcore/Mp | Rcore/Rp | ABond | Teq (K) | Tsurf (K) | τ | H (km) |
|---|---|---|---|---|---|---|---|---|---|---|
| MR-S |  |
 |
 |
 |
||||||
| Gl 486 b | MRA-S |  |
 |
 |
 |
See text | ||||
| MRA-S H |  |
 |
 |
 |
||||||
| Mercury | ~0.15 | ~0.85 | 0.828 ± 0.012 | 0.088 | 437 | … | … | … | ||
| Venus | −4.00 ± 0.01 | ~0.67 | ~0.33 | 0.525 ± 0.045 | 0.76 | 229 | 737 | 160 | 15.9 | |
| Earth | −3.62 ± 0.03 | ~0.67 | ~0.33 | 0.4536 ± 0.016 | 0.306 | 254 | 287 | 0.94 | 8.5 | |
| Mars | −7.41 ± 0.02 | ~0.85 | ~0.15 | 0.539 ± 0.012 | 0.250 | 210 | 213 | 0.09 | 11.1 |
Notes. All parameters from the NASA Fact Sheets or computed by us except for the core-to-mantle mass ratios of Solar System planets, which are actually the iron mass fraction estimated by Lodders & Fegley (1998). Actual Mercury Tsurf ranges from about 100 K on the dark side and at the bottom of deep craters to about 700 K at the sub-solar point during aphelion. (a)Models – MR-S: baseline model with water steam upper layer (894000 samples); MRA-S: MR-S plus stellar abundance constraints (725 000 samples); MRA-SH: MRA-S plus hydrated magma (224000 samples). Nomenclature follows the ‘data type-model setup’ structure.
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