Dependence of the Radiative-Convective Equilibrium Structure of the Lower Atmosphere of Venus on the Thermodynamic Model

Dependence of the radiative-convective equilibrium structure of the lower atmosphere of Venus on the speci-fication of an atmospheric thermodynamic model is investigated. A series of thermodynamic models including ideal gases, van der Waals gases, and real gases are introduced by the use of the Helmholtz energy given by the EOS-CG mixture model (EOS-CG: Equation of State for Combustion Gases and Combustion Gas-like Mixtures). It is demonstrated that the radiative-convective equilibrium profile for the real gas differs significantly from that for the ideal gas with temperature-dependent specific heat by an increase of about 7 K in the surface temperature. This difference is caused by the fact that the adiabatic lapse rate evaluated with the thermodynamic model of real gas is larger than that of ideal gas, since the non-ideality of gas increases the thermal expansion coefficient, which overwhelms the increases in density and specific heat. It is confirmed that, in order to obtain better calcu-lations of atmospheric circulations including the lower atmosphere of Venus, the ideal gas with a constant spe-cific heat should be abandoned. The ideal gas with a temperature-dependent specific heat may not be enough. A promising method is to use the ideal gas but with the temperature-dependent specific heat such that its adiabatic lapse rate profile mimics that for the real gas.