Table 1
Model parameters, helium line strengths extracted from observational papers, and the constrained temperatures and mass-loss rates for investigated exoplanets.
| Planet | R (Rj) | M (Mj) | log10(|ϕ|) (cgs) | a (AU) | SED | He λ 10 830 signal | T (K) |  (log10(g s−1 )) |
|---|---|---|---|---|---|---|---|---|
| HD 209458 b | 1.39 | 0.73 | 12.98 | 0.04747 | Salz et al. (2016) | 4.03 ± 0.55 mÅ (1) |  |
 |
| WASP-69 b | 1.057 | 0.26 | 12.65 | 0.04525 | HD 85512 (K6)(m) | 0.512 ± 0.049% (2) |  (u) |
 (u) |
| WASP-52 b | 1.27 | 0.46 | 12.82 | 0.0272 | є Eridani (K2)(m) | 40.3 ± 6.1 mÅ (3) |  |
 |
| HAT-P-11 b | 0.389 | 0.0736 | 12.53 | 0.053 | Avg. K2 & K6 (a) | 9.26 ± 1.82 mÅ (4) |  |
 |
| HAT-P-18 b | 0.995 | 0.197 | 12.55 | 0.0559 | є Eridani (K2)(m) | 0.70 ± 0.16% (5) |  |
 |
| WASP-107 b | 0.94 | 0.096 | 12.27 | 0.055 | HD 85512 (K6)(m) | 48.02 ± 10.78 mÅ (6) |  (u) |
 (u) |
Notes. (m)From the MUSCLES survey, version 2.2 (France et al. 2016; Youngblood et al. 2016; Loyd et al. 2016). (a)Averaged MUSCLES spectra of 6 Eridani (K2) and HD 85512 (K6). (1)EW from Alonso-Floriano et al. (2019). (2)Excess absorption from Vissapragada et al. (2022b). (3)EW from Kirk et al. (2022).(4)EW from Mansfield et al. (2018).(5)Excess absorption from Vissapragada et al. (2022b).(6)EW from Spake et al. (2018). (u)Underestimated uncertainty due to exceeding our modeled parameter space. The latter were inferred from Fig. 5.
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