Table 1
Numerical values used in the case of Venus-like planets.
| Parameters | Values | Units |
|
|
||
|
6.67384 × 10-11 | m3 kg-1 s-2 |
| ℛGP | 8.314 | J mol-1 K-1 |
| L ∗ | 3.846 × 1026 | W |
|
1.32712 × 108 | km3 s-2 |
| R | 6051.8 | km |
| M P | 4.8676 × 1024 | kg |
| f A | 10-4 | – |
| ℳA | 43.45 | g mol-1 |
| T 0 | 737 | K |
| κ | 0.286 | – |
| ω 0 | 3.77 × 10-7 | s-1 |
| α | 0.19 | – |
| β | 1.0 | – |
| ε | 0.04 | – |
| G | 1011 | Pa |
| ω M | 1.075 × 10-4 | s-1 |
Notes. Parameters from 
to T0 are given by Nasa fact sheets1 and Mohr et al. (2012), the value of κ corresponds to a perfect gas, ω0 is the radiative frequency prescribed by Leconte et al. (2015) for Venus, α is computed for a tidal heat power per unit mass proportional to cosΨ on the day side and equal to zero on the night side, the atmospheric tidal torque is assumed to be entirely transmitted to the telluric core (β = 1), ε is consistant with the estimation of Dobrovolskis & Ingersoll (1980) for the effective heating of Venus’ atmosphere by the ground, and we take for G the shear modulus of silicates (Remus et al. 2012).
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