An Enduring Rapidly Moving Storm as a Guide to Saturn's Equatorial Jet's Complex Structure

Abstract

Saturn has an intense and broad eastward equatorial jet with a complex three-dimensional structure mixed with time variability. The equatorial region experiences strong seasonal insolation variations enhanced by ring shadowing and three of the six known giant planetary-scale storms have developed in it. These factors make Saturn's equator a natural laboratory to test models of jets in giant planets. Here we report on a bright equatorial atmospheric feature imaged in 2015 that moved steadily at a high speed of 450 ms-1 not measured since 1980-81 with other equatorial clouds moving within an ample range of velocities. Radiative transfer models show that these motions occur at three altitude levels within the upper haze and clouds. We find that the peak of the jet (latitudes 10\degree N to 10\degree S) suffers intense vertical shears reaching +2.5 ms-1 km-1, two orders of magnitude higher than meridional shears, and temporal variability above 1 bar altitude level.

References in corpus (1)

• Dynamics of Saturn's great storm of 2010-2011 from Cassini ISS and RPWS

Cited by in corpus (4)

• Saturn atmospheric dynamics one year after Cassini: Long-lived features and time variations in the drift of the Hexagon
• Temporal and spatial variations of the absolute reflectivity of Jupiter and Saturn from 0.38 to 1.7 $\mu$m with PlanetCam-UPV/EHU
• Multilayer hazes over Saturn's hexagon from Cassini ISS limb images
• Mapping Saturn using deep learning