Atmospheric super-rotation

For instance, on Venus, the interaction of thermal tides with planetary-scale Rossby waves is thought to contribute significantly to its rapid super-rotational winds.

[2] Super-rotation present in the stratosphere of Titan has been inferred by Voyager IRIS, Cassini CIRIS, stellar occultation and temperature observations, and Doppler shifts of the Huygens probe’s radio signal.

Questions on the effect of obliquity in super-rotation on Titan is often compared to Venus, as they share similar centrifugal accelerations to achieve dynamic balance.

The first observations of Titan in the 1980's revealed little information about circulation within the atmosphere due to the low contrast photochemical haze covering the moon.

The first general circulation model (GCMs) in the 1990s provided insight into the stratospheric properties that should be expected on Titan with further observation, and predicted super-rotation with winds up to 200 m/s.

[6] Super-rotation was supported by the first 3D Titan GCM created by the Laboratoire de Météorologie Dynamique (LMD), in which they used an atmosphere similar to the observations of Voyager and recently Cassini.

[3] Comparing TitanWRF v2 simulations with constant solar forcing (seasonal cycle removed) models,[7] showed that in the latter, a rapid buildup in rotation, attaining > 100m/s, happened in a few Titan years.

These distant worlds, orbiting close to their stars, often exhibit extreme atmospheric conditions, including super-rotation, which influences their thermal structures and potential habitability.