Atmospheric CirculationVenus has winds that cause the atmosphere to rotate 60 times faster than the solid planet, in a phenomenon called “super-rotation”. The strong winds have an enormous impact on the planet´s climate. The simulation with 2 degrees reproduced strong winds that are largely consistent with the observations within the standard deviation. This represents a great success for the OASIS platform since 3D GCM simulations of the Venus circulation are very challenging (Sanchez-Lavega et al. 2017). The observational data in the figure (lines) was obtained from many observational campaigns to measure the wind velocity at the Venus clouds (Sanchez-Lavega et al. 2017). The dots represent average values at the altitude of the Venus clouds simulated by OASIS. The winds plotted correspond to an altitude range of 65-70 km. The model results were spatially averaged over the day-side hemisphere to be consistent with the UV observations and the uncertainties correspond to the standard deviation. The results were time-averaged over 1,000 Earth days. The colormap on the right shows how OASIS (rainbow colours) can spatially match the wind velocities to the cloud structure (copper colours) in the observations.
Temperature brightness from OASIS and observations from Venera 15 (Zasova et al. 2004). The solid lines are results from observations at different regions in the atmosphere (Zasova et al. 2004). The main absorption features from CO2, H2O, SO2 and H2SO4 are indicated in the Figure. The blue and red points are results from OASIS with a spatial resolution of 2 and 4 degrees respectively. The model results correspond to globally averaged values of the temperature brightness for different wavelengths. The uncertainties of the model values are the standard deviation of the globally averaged values.