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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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