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Table 2

Main quantities used in this paper.

Symbol Quantity Definition Units

κ R Rosseland mean opacities Eq. (2) m2/kg
κ P Planck mean opacities Eq. (5) m2/kg
κ 1 Opacity in the first band Eq. (8) m2/kg
κ 2 Opacity in the second band Eq. (8) m2/kg
β Relative width of the first band Eq. (9)
κ v Opacity in the visible Eq. (7) m2/kg
τ Rosseland optical depth Eq. (3)
R Opacity ratio κ1/κ2 Sect.3.4
γ1, γ2, γP, γv κ1/κR, κ2/κR, κP/κR, κv/κR Eqs. (12), (13), (6)and (7)
τ lim Limit optical depth Eq. (15) Hz
ν Frequency Hz
μ cosine of the direction angle θ
μ cosine of the angle between the vertical and the star
γv/μ
I μν Specific intensity at frequency ν and in the direction μ Chandrasekhar (1960) W/m2/Hz/sr
Jν, Hν, Kν First, second, and third momentum of the specific intensity Eq. (20) W/m2/Hz
J, H, K Integrated values of Jν, Hν, and Kν W/m2
Internal flux from the planet W/m2
Stellar flux arriving at the substellar point of the planet Sect. 3.7 W/m2
Stellar flux that penetrates the modelled atmospheric column W/m2
H i,irr Contribution of the irradiation to H transported by the ith Eq. (99) W/m2
thermal band
H i,int Contribution of the internal luminosity to H transported by the Eq. (99) W/m2
ith thermal band
T eff Effective temperature of the planet Sect. 2.1 K
T eff,   μ Effective temperature of the modelled atmosphere Sect. 2.1 K
T skin Temperature at optical depth of zero. K
T deep Temperature at large optical depth. Eq. (109) K
f Parameter used to calculate dayside and planetary averages Sect. 3.7

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