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Kelvin-Helmholtz instabilities are visible in the atmospheres of planets and moons, such as in cloud formations on Earth or the Red Spot on Jupiter, and the atmospheres of the Sun and other stars. [1] Spatially developing 2D Kelvin-Helmholtz instability at low Reynolds number. Small perturbations, imposed at the inlet on the tangential velocity ...
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.
The Taylor–Goldstein equation is an ordinary differential equation used in the fields of geophysical fluid dynamics, and more generally in fluid dynamics, in presence of quasi-2D flows. [1] It describes the dynamics of the Kelvin–Helmholtz instability , subject to buoyancy forces (e.g. gravity), for stably stratified fluids in the ...
The Kelvin–Helmholtz mechanism is an astronomical process that occurs when the surface of a star or a planet cools. The cooling causes the internal pressure to drop, and the star or planet shrinks as a result. This compression, in turn, heats the core of the star/planet.
It is a measure of relative importance of mechanical and density effects in the water column, as described by the Taylor–Goldstein equation, used to model Kelvin–Helmholtz instability which is driven by sheared flows.
A Kelvin-Helmholtz instability forms where there's a velocity difference across the interface between two fluids: for example, wind blowing over water.You’ll often see the characteristic wave ...
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.
In astrophysics, the thermal time scale or Kelvin–Helmholtz time scale is the approximate time it takes for a star to radiate away its total kinetic energy content at its current luminosity rate. [1]