Compare To Venus Observations

Atmospheric Circulation

The results of the model show winds in Venus at a velocity around 100 m/s, which is roughly 60x faster than the solid planet. 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 winds plotted correspond to an altitude range of 65-70 km. The observational values (lines in the figure) were estimated by tracking the cloud motions at UV wavelengths in multiple space missions (Sanchez-Lavega et al. 2017). The filled circles correspond to the OASIS results: red (simulation with 4 degrees spatial resolution) and black (simulation with 2 degrees spatial resolution). 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.

Temperature Brightness

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.