# Kelvin–Helmholtz instability

(Redirected from Kelvin-Helmholtz instability)
Numerical simulation of a temporal Kelvin–Helmholtz instability

The Kelvin–Helmholtz instability (after Lord Kelvin and Hermann von Helmholtz) is a fluid instability that occurs when there is velocity shear in a single continuous fluid or a velocity difference across the interface between two fluids. 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, evolve in the computational box. High Reynolds number would be marked with an increase of small scale motions.

## Theory overview and mathematical concepts

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

Fluid dynamics predicts the onset of instability and transition to turbulent flow within fluids of different densities moving at different speeds.[3] If surface tension is ignored, two fluids in parallel motion with different velocities and densities yield an interface that is unstable to short-wavelength perturbations for all speeds. However, surface tension is able to stabilize the short wavelength instability up to a threshold velocity.

If the density and velocity vary continuously in space (with the lighter layers uppermost, so that the fluid is RT-stable), the dynamics of the Kelvin-Helmholtz instability is described by the Taylor–Goldstein equation: ${\displaystyle (U-c)^{2}\left({d^{2}{\tilde {\phi }} \over dz^{2}}-k^{2}{\tilde {\phi }}\right)+\left[N^{2}-(U-c){d^{2}U \over dz^{2}}\right]{\tilde {\phi }}=0,}$ where ${\displaystyle N={\sqrt {g \over L_{\rho }}}}$ denotes the Brunt–Väisälä frequency, U is the horizontal parallel velocity, k is the wave number, c is the eigenvalue parameter of the problem, ${\displaystyle {\tilde {\phi }}}$ is complex amplitude of the stream function. Its onset is given by the Richardson number ${\displaystyle \mathrm {Ri} }$. Typically the layer is unstable for ${\displaystyle \mathrm {Ri} <0.25}$. These effects are common in cloud layers. The study of this instability is applicable in plasma physics, for example in inertial confinement fusion and the plasmaberyllium interface. In situations where there is a state of static stability, evident by heavier fluids found below than the lower fluid, the Rayleigh-Taylor instability can be ignored as the Kelvin–Helmholtz instability is sufficient given the conditions.[clarification needed]

Numerically, the Kelvin–Helmholtz instability is simulated in a temporal or a spatial approach. In the temporal approach, the flow is considered in a periodic (cyclic) box "moving" at mean speed (absolute instability). In the spatial approach, simulations mimic a lab experiment with natural inlet and outlet conditions (convective instability).