Venus Thermospheric CirculationThe adopted approach has been to re-examine the circulation by first using the previous two-dimensional code to quantify those physical processes which can be inferred from the Pioneer Venus observations. Specifically, the model was used to perform sensitivity studies to determine the degree to which eddy cooling, eddy or wave drag, eddy diffusion and 15 (mu)m radiational cooling are necessary to bring the model temperature and composition fields into agreement with observations. Three EUV heating cases |
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airglow altitude benchmark BNMS Chapter CO₂ composition and temperature day-night dayside density scale heights Dickinson 1976 Dickinson and Ridley diurnal DRM1 and DRM2 DRM2 dynamical eddy cooling eddy diffusion eddy drag eddy mixing emission empirical model energy equations EUV heating efficiency exospheric temperatures fluxes FRACTIONAL NUMBER DENSITY global mean temperature gravity waves Hedin horizontal winds HSYM hydrodynamic hydrodynamic model improved Keating Kg(z KMAX lower boundary Massie Mayr mesosphere mixing ratios model simulation momentum Niemann night side nightside nightside temperatures one-dimensional model ONMS orbiter parameterizations parameters perturbation photodissociation Pioneer Venus observations Pioneer Venus orbiter pressure rate coefficient Rayleigh friction Section Seiff self-consistent sensitivity study sition solar maximum specifically spectrometer Stewart subsolar-to-antisolar super-rotating temperature profiles TGCM thermal balance thermodynamic equation thermospheric circulation three-dimensional turbopause upper atmosphere values variation velocities Venus thermosphere Venus two-dimensional model vertical VTGCM VTS3 wave drag wind fields Zahn ZPBK