Kelvin-Helmholtz instability

This can produce Kelvin-Helmholtz instability, resulting in a turbulence which leads to mixing.

This process is often described and modelled as an example of Kelvin-Helmholtz instability, though other processes may play a role as well.

The shear produces a Kelvin-Helmholtz instability that forms spiral-shaped patterns.

In this case a statistical study of the data indicates that a Kelvin-Helmholtz instability would be the triggering mechanism.

In particular, they may exhibit Kelvin-Helmholtz instability.

Coherent structures form due to some sort of instability, e.g. the Kelvin-Helmholtz instability.

For example, when two layers of fluid shear against each other with relative velocity, the Kelvin-Helmholtz instability may occur.

Kelvin-Helmholtz instability (similar, but different from the diocotron instability in plasmas)

This instability is the plasma analog of the Kelvin-Helmholtz instability in fluid mechanics.

It was readily known that such steady flows are not stable, since the vortex sheets develop so-called Kelvin-Helmholtz instabilities.

The interaction of the stellar wind with the surrounding cloud also forms "waves" which are believed to be due to the hydrodynamical Kelvin-Helmholtz instability.

HVCs in the galactic halo are destroyed through what is called the Kelvin-Helmholtz instability.

His PhD work led to the first direct evidence for Kelvin-Helmholtz instability at the Earth's magnetopause.

However, from a dynamical point of view, a better analogy is with the Kelvin-Helmholtz instability, or with beads sliding along an oscillating string.

This motion causes the appearance of a series of overturning ocean waves, a characteristic of the Kelvin-Helmholtz instability.

The Kelvin-Helmholtz instability (KHI) is an application of hydrodynamic stability that can be seen in nature.

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.

The scientists propose the physics governing these deformations is similar to phenomena seen in clouds, the sea and other turbulent fluids known as the "Kelvin-Helmholtz Instability."

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.

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.

Surfer waves — initiated in the sun, as they are in the water, by a process called a Kelvin-Helmholtz instability — have been found in the sun's atmosphere.

The nonlinear Kelvin-Helmholtz instability of a horizontal interface between a magnetic inviscid incompressible liquid and an inviscid laminar subsonic gas is investigated.

Kelvin-Helmholtz instabilities occur when large swirls of plasma travel along the edge of the magnetosphere at a different velocity from the magnetosphere, causing the plasma to slip past.

Long period (1-10 mHz) waves generated by boundary layer instability processes such as the Kelvin-Helmholtz instability, have been found to couple to field line resonances at plasmatrough latitudes.

Another example of the Kelvin-Helmholtz instability are waves that grow on jets of high or low density fluid, such as the hot bouyant jet of gas shown in example 4b (132K).