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The atmosphere of Venus is characterized by strong superrotation, in whichthe wind velocities at cloud heights are around 60 times faster than thesurface rotation rate. The reasons for this strong superrotation are still notwell understood. Motions in the atmosphere below the thick cloud deck are hardto determine remotely and in-situ measurements of the circulation below 40 kmaltitude are scarce. No model to date has been able to simulate superrotatingwinds with magnitudes comparable with those measured by entry probes, in thedense atmosphere between the surface and the clouds. However, importantinformation on the dynamics and circulation of Venus' atmosphere can bedetermined by studying the atmosphere at cloud levels, where there aresignificantly more measurements than in the sub-cloud region, including themany recent observations made during the Venus Express and Akatsuki missions.In this work we describe a new Venus Middle atmosphere general circulationModel (VMM) to study the dynamics of the atmosphere at cloud altitudes. Themodel simulates the atmosphere from just below cloud deck to around 95 kmaltitude. We present simulations using the VMM with a simplified Newtoniancooling radiation scheme. Sensitivity studies have been performed to determinethe most appropriate values for model parameters and the model has beenvalidated by comparison with observations, including those from Venus Expressand Akatsuki. The validated model provides some constraints on parameters whichare poorly measured close to the boundary such as the mean winds andtemperatures, and provides a basis for further investigations of the dynamicsof Venus' cloud-level atmosphere. In future studies we will also investigatethe influence of atmospheric waves, such as Kelvin and Rossby waves, todetermine the role they play in generating the poorly-understood cloud-levelstructure at all latitudes.

Simulating Venus' Cloud Level Dynamics Using a Middle Atmosphere General Circulation Model