Table 1
Nearby planet sample.
| log ϕp (1) | ρp(2) | log(FXUV) (3) | log(Ṁ) (4) | |
|---|---|---|---|---|
| 55 Cnc e | 12.44 | 6.67 | 4.37 | 10.59 |
| GJ 1214 b | 12.15 | 1.57 | 3.30 | 10.09 |
| GJ 3470 b | 12.30 | 0.82 | 3.67 | 10.65 |
| GJ 436 b | 12.57 | 2.15 | 3.13 | 9.79 |
| GJ 9827 b | 12.16 | 4.20 | 3.80 | 10.17 |
| GJ 9827 d | 12.23 | 3.05 | 2.85 | 9.42 |
| HAT-P-11 b | 12.52 | 1.19 | 3.52 | 10.41 |
| HD 149026 b | 12.84 | 0.86 | 3.98 | 11.08 |
| HD 189733 b | 13.27 | 0.91 | 4.38 | 9.99 |
| HD 209458 b | 12.97 | 0.33 | 3.03 | 10.46 |
| HD 97658 b | 12.42 | 4.78 | 2.82 | 9.24 |
| K2−25 b | 12.70 | 3.01 | 4.06 | 10.44 |
| WASP-43 b | 13.56 | 2.40 | 4.62 | 7.97 |
| WASP-69 b | 12.65 | 0.27 | 4.00 | 11.50 |
| WASP-77 A b | 13.40 | 1.12 | 4.57 | 9.60 |
| WASP-80 b | 13.02 | 0.69 | 3.77 | 10.57 |
Notes. Specific gravitational potential energy (1); mean mass density (2); XUV flux at the planet orbital distance (3); mass outflow rate (4). Stellar and orbital parameters have been revised to account for the recently revised Gaia DR2 distances (Gaia Collaboration 2018); X-ray fluxes were estimated from the original (Chandra or XMM-Newton) data adopting a homogeneous data reduction, and fluxes at the planet orbital distance were calculated adopting the X-ray to XUV scaling relations by King et al. (2018). The ensuing mass outflow rates are derived using ATES (Caldiroli et al. 2021). From Spinelli et al. (Paper III of this series, in prep.). All quantities are expressed in cgs units.
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