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Making waves.These images taken on Aug. 18 (left) and Aug. 27 (right), 2016, by the near-infrared camera on Japan’s Akatsuki Venus probe, show the clear line of denser (darker) clouds moving across the planet.
Image Credit: ©T. Imamura, Y. Maejima, K. Sugiyama et al., 2026
(CC BY 4.0)
Scientific Frontline: Extended "At a Glance" Summary: Venusian Atmospheric Hydraulic Jumps
The Core Concept: A Venusian atmospheric hydraulic jump is an abrupt slowing and deepening of a fast-moving atmospheric fluid, which creates a massive 6,000-kilometer-wide wave front in the planet's cloud layer. It forces sulfuric acid vapor upward, condensing it into a distinctly visible, planetary-scale line of cloud.
Key Distinction/Mechanism: While typical atmospheric models treat large-scale horizontal processes and localized vertical waves as disconnected, this Venusian phenomenon uniquely links an unstable eastward-moving Kelvin wave with a severe vertical updraft. As wind speed abruptly drops, it creates the largest known hydraulic jump in the solar system, mechanically similar to the sudden transition from fast, shallow water to slow, deep ripples in a basin.
Major Frameworks/Components:
- Fluid Dynamic Models: Numerical analyses used to simulate the gas and liquid flow dynamics of the planetary-scale jump.
- Microphysical Box Models: Simulations tracking the behavior and condensation of sulfuric acid vapor as it moves vertically through the atmosphere.
- Kelvin Waves: Large-scale, eastward-moving atmospheric waves in the lower and middle cloud layers that become unstable and trigger the hydraulic jump.
- Superrotation Maintenance: The underlying mechanism by which the Venusian atmosphere rotates approximately 60 times faster than the planet itself, a process bolstered by these atmospheric disturbances.


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