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A KH instability rendered visible by clouds, known as fluctus, [2] over Mount Duval in Australia A KH instability on the planet Saturn, formed at the interaction of two bands of the planet's atmosphere Kelvin-Helmholtz billows 500m deep in the Atlantic Ocean Animation of the KH instability, using a second order 2D finite volume scheme
This is an image, captured in San Francisco, which shows the "ocean wave" like pattern associated with the Kelvin–Helmholtz instability forming in clouds. The Kelvin–Helmholtz instability (KHI) is an application of hydrodynamic stability that can be seen in nature. It occurs when there are two fluids flowing at different velocities.
Görtler instability: Stability of flow along a concave boundary layer: H. Görtler: Holmboe instability: Stratified shear flows: Jørgen Holmboe: Jeans instability: Stability of interstellar gas clouds: James Jeans: Kelvin–Helmholtz instability: Stability of shearing flow: Lord Kelvin and Hermann von Helmholtz: Kruskal–Shafranov ...
A curious cloud seen over Smith Mountain looks more like something out of a fairytale than it does real life — and the science behind it is fascinating. What are Kelvin-Helmholtz clouds?
Kelvin–Helmholtz instability can occur when velocity shear is present within a continuous fluid or when there is sufficient velocity difference across the interface between two fluids. Rossby waves (or planetary waves) are large-scale motions in the atmosphere whose restoring force is the variation in Coriolis effect with latitude.
Depending on the size of the velocity difference and the size of the density contrast between the layers, Kelvin-Helmholtz waves can look different. For instance, between two layers of air or two layers of water, the density difference is much smaller and the layers are miscible; see black-and-white model video.
Hydrodynamics simulation of a single "finger" of the Rayleigh–Taylor instability. [1] Note the formation of Kelvin–Helmholtz instabilities, in the second and later snapshots shown (starting initially around the level =), as well as the formation of a "mushroom cap" at a later stage in the third and fourth frame in the sequence.
It describes the dynamics of the Kelvin–Helmholtz instability, subject to buoyancy forces (e.g. gravity), for stably stratified fluids in the dissipation-less limit. Or, more generally, the dynamics of internal waves in the presence of a (continuous) density stratification and shear flow.