[PPS06-P10] A sensitivity study of the radiative-convective equilibrium temperature profile in Venus atmosphere
Keywords:Venus, Radiative transfer model, Radiative-convective equilibrium
To better knowledge on the thermal structure (radiative transfer of the thermal flux), we calculated the radiative-convective equilibrium temperature profile of Venus atmosphere using a newly developed 1-D radiative transfer model “MSTRN-Venus”. The absorption coefficients of the molecular gases in the Venus atmosphere (CO2, H2O, CO, SO2, HF, HCl, and OCS) are calculated in each 0.025cm-1 wavenumber and correlated k-distribution are calculated and applied. The spectroscopic parameters such as the transition position and line strength are taken from the recent compilations of HITRAN, HITEMP, and UCL08 catalogs. In addition, the collision-induced absorption of CO2 is also included. We prepared the absorption coefficients under several pressure and temperature conditions within the ranges of 0.01 - 100 bar and 100 - 800 K, respectively. The results are kept in a look-up table of (p, T) domain so that we can interpolate the absorption coefficient for any pressure and temperature condition without repeating a burden computation. The upward and downward flux density is calculated for a given atmospheric profile using the MSTRN code. This code has been successfully applied in several studies of our terrestrial atmosphere, and also adopted as the radiation calculation module of several general atmospheric circulation models.
The presentation will discuss the sensitivity of the radiative-convective temperature profile concerning the abundance of minor species, incoming solar heating, and cloud opacities.