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Examination of amateur observations of Mars shows atmospheric plumes 200 to 250 kilometres high that are observed in the morning but not in the evening over a period of more than a week; our current understanding of Martian atmospheric dynamics and plume formation cannot account for the creation of such enormous plumes.

Calculations show that severe methane convective storms accompanied by intense precipitation may occur on Titan under the right environmental conditions. Such rainfalls on Titan's surface are comparable to flash flood events on Earth.

The SuperCam microphone aboard the Perseverance rover captured 55 triboelectric discharges during dust events on Mars over two Martian years, providing implications for examining the planet’s surface chemistry, habitability and human exploration.

The atmospheres of most planets in our Solar System have a single large cyclonic vortex at each of their poles. Jupiter with its polygonal cyclones surrounding a single one, however, falls out of line, owing to an energy transfer to larger scales.

The authors analyze a system of multi-layered hazes above Saturn’s hexagonal-wave cloud tops in the visual range. Analyses suggest the formation to be caused by condensation processes, and the vertical distribution of stacked layers by the upward propagation of internal gravity waves.

James Webb Space Telescope observations of Jupiter have unveiled the presence of a narrow and intense atmospheric jet in the equator of the planet near the tropopause. The jet’s speed of 500 km h⁻¹ doubles the speed of the lower clouds. This new jet aligns with temperature and wind oscillations in Jupiter’s stratosphere.

The visible–near-infrared spectrum of the dark spot that appeared on Neptune in 2018 indicates the presence of material that makes the aerosol layer at 5 bar darker at visible wavelengths. Such material can come from deeper layers via upwelling or by sublimation of H₂S ice that reveals the darker condensation nuclei.

Observations and modelling of two plumes in Jupiter's atmosphere that erupted at the same latitude as the strongest jet (23° North) are reported. Based on dynamical modelling it is concluded that the data are consistent only with a wind that extends well below the level where solar radiation is deposited.

The origin, variability, and structure of Saturn’s intense and broad eastward equatorial jet at upper cloud level are complex and unexplained. Here, based on observations of a large, bright equatorial disturbance in 2015, the authors characterise the vertical structure of the jet and its long-term variability.

A series of four storms appeared on Saturn’s northern polar region in 2018, unusually close to each other in space and time. By their dimension and the energy needed to form them, they appear to be a hitherto unobserved kind of storm at Saturn, intermediate between the regional- and the global-sized ones.