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Venus is covered by thick clouds that move with the prevailing winds. Images from JAXA’s Akatsuki orbiter taken in July 2016 reveal more variability deep in the cloud layer than expected, including a feature consistent with an equatorial jet.
The Martian atmosphere hosts water-ice clouds, but it is thought that any snow precipitation settles slowly, rather than in storms. Martian meteorology simulations suggest that localized convective snowstorms can occur on Mars during the night.
Ancient Mars may have had an active sulfur cycle. In situ analyses by the Curiosity rover reveal large variations in the current sulfur isotopic composition of Martian sediments that can be explained by geologic and atmospheric processes.
Venus Express wind measurements at Venus’s cloud top during the night show a different picture than dayside. Both fast and slow motions are detected (there are only fast ones during the day) as well as many stationary waves related to surface relief.
Volcanic glasses sampled by Apollo missions display high water contents. Remotely sensed spectral data show that pyroclastic deposits are generally enriched in water across the Moon, suggesting significant amounts of water in the lunar interior.
Most of the Mars Trojans — asteroids co-orbiting the planet — are dynamically related; thus, they have a common origin. Joint information from spectral observations and dynamical modelling suggests that they were ejected from Mars itself after an impact.
A fast equatorial jet in the Venusian cloud layer has been revealed by the Akatsuki orbiter by tracking cloud movement in near-infrared images. The findings suggest that the Venusian atmosphere is more variable than previously thought.
Even though a thick atmosphere stands between Venus's cloud top and its surface, recent observations now establish the impact of Venus's topography on its upper atmospheric dynamics. Understanding how this is possible will lead to substantial progress in atmospheric computer models.