The Rayleigh-Taylor instability extracts gravitational potential energy when a heavy fluid is supported above a lighter one. A small downward excursion of heavy material and upward excursion of light material can grow instead of experiencing restoring buoyancy. The Kelvin-Helmholtz instability instead extracts kinetic energy from a velocity difference across an interface or shear layer. The interface displacement and its induced flow reinforce one another by tapping the background shear; a reversed density ordering is not required.
A useful common model has two inviscid, incompressible, semi-infinite fluids separated at , with lower density/velocity , upper density/velocity , downward gravity , and surface tension . For a disturbance proportional to , with , the two-fluid interfacial gravity-shear dispersion relation isA negative right side gives exponential growth. With no shear or surface tension and , the growth rate of the Rayleigh-Taylor instability is , where is the Atwood number. With equal densities and no restoring force, the growth rate of the Kelvin-Helmholtz instability is . Heavy-over-light stratification drives Rayleigh-Taylor growth; velocity shear drives Kelvin-Helmholtz growth. A heavy lower fluid supplies gravitational stabilization, and surface tension stabilizes sufficiently short waves in this ideal interface model.
Finite shear-layer thickness, viscosity, compressibility and magnetic tension can change the growth rates and unstable wavelength range. In particular, unlimited growth with increasing is a limitation of the zero-thickness, zero-surface-tension idealization. Density-interface overturning and jet-boundary mixing are appropriate physical applications of the two mechanisms, but the nonlinear mixed state is not determined by the linear growth rate alone.
Original schematics of Rayleigh-Taylor instability and Kelvin-Helmholtz instability
. Details. Articles by others on the same topic
There are currently no matching articles.
