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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 ...
The Kelvin–Helmholtz instability can be seen in the bands in planetary atmospheres such as Saturn and Jupiter, for example in the giant red spot vortex. In the atmosphere surrounding the giant red spot there is the biggest example of KHI that is known of and is caused by the shear force at the interface of the different layers of Jupiter's ...
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.
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 ...
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 ...
In particular, they may exhibit Kelvin–Helmholtz instability. The formulation of the vortex sheet equation of motion is given in terms of a complex coordinate z = x + i y {\displaystyle z=x+iy} . The sheet is described parametrically by z ( s , t ) {\displaystyle z(s,t)} where s {\displaystyle s} is the arclength between coordinate z ...
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 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.