Richtmyer–Meshkov instability

The Richtmyer–Meshkov instability (RMI) occurs when two fluids of different density are impulsively accelerated. Normally this is by the passage of a shock wave. The development of the instability begins with small amplitude perturbations which initially grow linearly with time. This is followed by a nonlinear regime with bubbles appearing in the case of a light fluid penetrating a heavy fluid, and with spikes appearing in the case of a heavy fluid penetrating a light fluid. A chaotic regime is reached eventually and the two fluids mix.

This instability can be considered the impulsive-acceleration limit of the Rayleigh–Taylor instability.^[1]

R. D. Richtmyer provided a theoretical prediction,^[2] and E. E. Meshkov (Евгений Евграфович Мешков)^(ru) provided experimental verification.^[3] Materials in the cores of stars, like Cobalt-56 from Supernova 1987A were observed earlier than expected. This was evidence of mixing due to Richtmyer–Meshkov and Rayleigh–Taylor instabilities. ^[4]

Here are the dispersion relations for ideal magnetohydrodynamics (MHD):

${\displaystyle (\omega ^{2}-2k_{\parallel }^{2}/\beta )(\omega ^{4}-(2/\beta +1)k^{2}\omega ^{2}+2k_{\parallel }^{2}k^{2}/\beta )=0}${\displaystyle (\omega ^{2}-2k_{\parallel }^{2}/\beta )(\omega ^{4}-(2/\beta +1)k^{2}\omega ^{2}+2k_{\parallel }^{2}k^{2}/\beta )=0}

For Hall MHD:

${\displaystyle {\displaystyle (\omega ^{2}-2k_{\parallel }^{2}/\beta )(\omega ^{4}-(2/\beta +1)k^{2}\omega ^{2}+2k_{\parallel }^{2}k^{2}/\beta )-2d_{s}^{2}k_{\parallel }^{2}k^{2}\omega ^{2}(\omega ^{2}-k^{2})/\beta =0}}${\displaystyle {\displaystyle (\omega ^{2}-2k_{\parallel }^{2}/\beta )(\omega ^{4}-(2/\beta +1)k^{2}\omega ^{2}+2k_{\parallel }^{2}k^{2}/\beta )-2d_{s}^{2}k_{\parallel }^{2}k^{2}\omega ^{2}(\omega ^{2}-k^{2})/\beta =0}}

For QMHD:

${\displaystyle {\displaystyle {\displaystyle ((1+2/\beta c^{2})\omega ^{2}-2k_{\parallel }^{2}/\beta )((1+2/\beta c^{2})\omega ^{4}-(2/\beta +1)k^{2}\omega ^{2}+2k_{\parallel }^{2}k^{2}/\beta )-2d_{s}^{2}k_{\parallel }^{2}k^{2}\omega ^{2}(\omega ^{2}-k^{2})/\beta =0}}}${\displaystyle {\displaystyle {\displaystyle ((1+2/\beta c^{2})\omega ^{2}-2k_{\parallel }^{2}/\beta )((1+2/\beta c^{2})\omega ^{4}-(2/\beta +1)k^{2}\omega ^{2}+2k_{\parallel }^{2}k^{2}/\beta )-2d_{s}^{2}k_{\parallel }^{2}k^{2}\omega ^{2}(\omega ^{2}-k^{2})/\beta =0}}}

During the implosion of an inertial confinement fusion target, the hot shell material surrounding the cold D–T fuel layer is shock-accelerated. This instability is also seen in magnetized target fusion (MTF).^[5] Mixing of the shell material and fuel is not desired and efforts are made to minimize any tiny imperfections or irregularities which will be magnified by RMI.

Supersonic combustion in a scramjet may benefit from RMI as the fuel-oxidants interface is enhanced by the breakup of the fuel into finer droplets. Also in studies of deflagration to detonation transition (DDT) processes show that RMI-induced flame acceleration can result in detonation.

• Rayleigh–Taylor instability
• Mushroom cloud
• Plateau–Rayleigh instability
• Salt fingering
• Kármán vortex street
• Kelvin–Helmholtz instability
• Hydrodynamics

• Mikaelian, Karnig O. (1985年01月01日). "Richtmyer–Meshkov instabilities in stratified fluids". Physical Review A. 31 (1). American Physical Society (APS): 410–419. Bibcode:1985PhRvA..31..410M. doi:10.1103/physreva.31.410. ISSN 0556-2791. PMID 9895490. S2CID 21139629.

• Wisconsin Shock Tube Laboratory
• New type of interface evolution in the Richtmyer–Meshkov instability
• Recent Advances in Indirect Drive ICF Target Physics at LLNL
• Emergence of Detonation in the Flowfield Induced by Richtmyer–Meshkov Instability
• Propagation of Fast Deflagrations and Marginal Detonations in Hydrogen-Air Mixtures
• Mushrooms+Snakes: a visualization of Richtmyer–Meshkov instability
• Conjugate Filter OscillationReduction (CFOR) scheme for the 2D Richtmyer–Meshkov instability
• Experiments on the Richtmyer–Meshkov instability at the University of Arizona Archived 2006年12月30日 at the Wayback Machine

• Fluid dynamics
• Plasma instabilities
• Astrophysics
• Fluid dynamic instabilities

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