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Table 1

Stellar and planetary model parameters.

Planet R (R) T (K) star spectrum a (AU) Mp (M) Rp (R) fi Tint (K) Atmosphere chemical composition
WASP-33b 1.444 a 7400 a,e 0.02565 j 667.4 m 17.97 p 1 300 H:He:C:N:O:S:P:Si:Ti solar × 10 q,r
HD 209458b 1.203 b 6092 b,f 0.04747 k 226.9 k 15.468 k 1/2 300 H:He:C:N:O:S:P:Si:Ti solar q,s
HD 189733b 0.805 b 4875 b,g 0.031l 371.9l 12.902 b 1/2 300 H:He:C:N:O:S:P:Si:Ti solar q,t
GJ 436b 0.464c 3684 c,h 0.02887 k 18.55 n 3.645 n 1/2 300 H:He:C:N:O:S:P solar × 100 q,u)
GJ 1214b 0.216d 3026 d,i 0.01411 d 8.17 o 2.742 o 1/2 300 H:He:C:N:O:S:P solar × 1000 q,v
CO2/N2 hot 1.0 4875 b,g 0.1 1.0 1.0 1/2 50 CO2:N2 1:1
H2O/CO2 cool 1.0 4875 b,g 1.0 1.0 1.0 1/2 50 H2O:CO2 1:1
volcano hot 1.0 4875 b,g 0.1 1.0 1.0 1/2 50 H2:H2O:CO:CO2:N2:H2S:SO2 1:1:1:1:1:1:1
N2/CH4 hot 1.0 4875 b,g 0.1 1.0 1.0 1/2 50 N2:CH4 1:1
N2/O2 warm 1.0 4875 b,g 0.3 1.0 1.0 1/2 50 N2:O2 1:1

Notes. – R and T are the stellar radius and effective temperature, respectively, a is the planet-star distance, Mp and Rp are the planetary mass and radius, respectively, fi is the factor by which the insolation is reduced to compute the dayside temperature as a result of the redistribution of heat from the dayside to the nightside (it takes a value of 1.0 for no redistribution from the dayside to the nightside and 0.5 for full redistribution between dayside and nightside), and Tint is the Stefan-Boltzmann temperature associated with the internal heat flux of the planet. aCollier Cameron et al. (2010). bBoyajian et al. (2015). cTorres (2007). dHarpsøe et al. (2013). e0.001–0.3 µm: WASP-17 MUSCLES14 spectrum (Behr et al. 2023); 0.3–160 µm: Castelli-Kurucz16 spectrum (Castelli & Kurucz 2004) for Teff = 7500 K, log g = 4.5, [M/H] = 0.0 scaled to Teff = 7400 K; 160–1000 µm blackbody spectrum. f 0.00005–0.168 µm: Sun spectrum (WHI; Woods et al. 2009); 0.168–300 µm: HD 209458 Kurucz15 spectrum scaled from Teff = 6100 to 6092 K; 300–1000 µm blackbody spectrum. g0.00051–0.335 µm: ϵ Eridani spectrum (provided by I. Ribas, see Venot et al. 2012); 0.335–300 µm: HD 189733 Kurucz15 spectrum scaled from Teff = 5050 to 4875 K; 300–1000 µm blackbody spectrum. h0.00055–5.5 µm: GJ 436 MUSCLES14 spectrum (France et al. 2016; Youngblood et al. 2016; Loyd et al. 2016), gap in range 0.16725–0.18065 µm filled with a uniform brightness of 10−11 erg s−1 cm−2 Hz−1 sr−1; 5.5–160 µm: Castelli-Kurucz16 spectrum (Castelli & Kurucz 2004) for Teff = 3750 K, log g = 5.0, [M/H] = 0.5 scaled to Teff = 3684 K; 160–1000 µm blackbody spectrum. i0.00055–5.5 µm: GJ 1214 MUSCLES14 spectrum (France et al. 2016; Youngblood et al. 2016; Loyd et al. 2016), gap in range 0.13375–0.18155 µm filled with a uniform brightness of 10−11 erg s−1 cm−2 Hz−1 sr−1; 5.5–160 µm: Castelli-Kurucz16 spectrum (Castelli & Kurucz 2004) for Teff = 3500 K, log g = 5.0, [M/H] = +0.5 scaled to Teff = 3026 K; 160–1000 µm blackbody spectrum. jSmith et al. (2011). kSouthworth (2010). lParedes et al. (2021). mLehmann et al. (2015). nMelo et al. (2024). oCloutier et al. (2021). pHardy et al. (2015). qAsplund et al. (2009). rCont et al. (2022). sXue et al. (2024). tFinnerty et al. (2024). uMukherjee et al. (2025b). vSchlawin et al. (2024).

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