Rayleigh–Taylor instability

Rayleigh–Taylor instability

The Rayleigh–Taylor instability, or RT instability (after Lord Rayleigh and G. I. Taylor), is an instability of an interface between two fluids of different densities, which occurs when the lighter fluid is pushing the heavier fluid. [citation
author=Sharp, D.H.
title=An Overview of Rayleigh-Taylor Instability
journal=Physica D
] Drazin (2002) pp. 50–51.] This is the case with an interstellar cloud and shock system. The equivalent situation occurs when Earth's gravity is acting on two fluids of different density — with the dense fluid above a fluid of lesser density — such as a denser-than-water oil floating above water.

Consider two completely plane-parallel layers of immiscible fluid, the heavier on top of the light one and both subject to the Earth's gravity. The equilibrium here is unstable to certain perturbations or disturbances. An unstable disturbance will grow and lead to a release of potential energy, as the heavier material moves down under the (effective) gravitational field, and the lighter material is displaced upwards. This was the set-up as studied by Lord Rayleigh. The important insight by G. I. Taylor was, that he realised this situation is equivalent to the situation when the fluids are accelerated (without gravity), with the lighter fluid accelerating into the heavier fluid. This can be experienced, for example, by accelerating a glass of water downward faster than the Earth's gravitational acceleration.

As the instability develops, downward-moving irregularities ('dimples') are quickly magnified into sets of inter-penetrating Rayleigh–Taylor fingers. Therefore the Rayleigh–Taylor instability is sometimes qualified to be a fingering instability. [citation | first1=H. B. | last1=Chen | first2=B. | last2=Hilko | first3=E. | last3=Panarella | title=The Rayleigh–Taylor instability in the spherical pinch | journal=Journal of Fusion Energy | volume=13 | issue=4 | year=1994 | doi=10.1007/BF02215847 | pages=275–280 ] The upward-moving, lighter material behaves like "mushroom caps". [cite arxiv | author=Wang, C.-Y. & Chevalier R. A. | title=Instabilities and Clumping in Type Ia Supernova Remnants | eprint=astro-ph/0005105 | year=2000 | version=v1 | accessdate=2008-10-10 ] [citation | contribution=Supernova 1987a in the Large Magellanic Cloud | first1=W. | last1=Hillebrandt | first2=P. | last2=Höflich | title=Stellar Astrophysics | editor=R. J. Tayler | publisher=CRC Press | year=1992 | isbn=0750302003 | pages=249–302 . See page 274.]

This process is evident not only in many terrestrial examples, from salt domes to weather inversions, but also in astrophysics and electrohydrodynamics. RT fingers are especially obvious in the Crab Nebula, in which the expanding pulsar wind nebula powered by the Crab pulsar is sweeping up ejected material from the supernova explosion 1000 years ago.citation
last = Hester | first = J. Jeff
year = 2008
title = The Crab Nebula: an Astrophysical Chimera
journal = Annual Review of Astronomy and Astrophysics
volume = 46
pages = 127–155
doi = 10.1146/annurev.astro.45.051806.110608

Note that the RT instability is not to be confused with the Rayleigh instability (or Plateau-Rayleigh instability) of a liquid jet. This latter instability, sometimes called the hosepipe (or firehose) instability, occurs due to surface tension, which acts to break a cylindrical jet into a stream of droplets having the same volume but lower surface area.

Linear stability analysis

The inviscid two-dimensional Rayleigh–Taylor (RT) instability provides an excellent springboard into the mathematical study of stability because of the exceptionally simple nature of the base state.Drazin (2002) pp. 48–52.] This is the equilibrium state that exists before any perturbation is added to the system, and is described by the mean velocity field U(x,z)=W(x,z)=0,, where the gravitational field is extbf{g}=-ghat{ extbf{z., An interface at z=0, separates the fluids of densities ho_G, in the upper region, and ho_L, in the lower region. In this section it is shown that when the heavy fluid sits on top, the growth of a small perturbation at the interface is exponential, and takes place at the rate

: ext{e}^{sqrt{mathcal{A}galpha},t},qquad ext{with}quad mathcal{A}=frac{ ho_{ ext{heavy- ho_{ ext{light}{ ho_{ ext{heavy+ ho_{ ext{light},,

where alpha, is the spatial wavenumber and mathcal{A}, is the Atwood number.

hidden begin
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title = Details of the linear stability analysis [A similar derivation appears in Chandrasekhar (1981), §92, pp. 433–435.]
The perturbation introduced to the system is described by a velocity field of infinitesimally small amplitude, (u'(x,z,t),w'(x,z,t))., Because the fluid is assumed incompressible, this velocity field has the streamfunction representation

: extbf{u}'=(u'(x,z,t),w'(x,z,t))=(psi_z,-psi_x),,

where the subscripts indicate partial derivatives. Moreover, in an initially stationary incompressible fluid, there is no vorticity, and the fluid stays irrotational, hence abla imes extbf{u}'=0,. In the streamfunction representation, abla^2psi=0., Next, because of the translational invariance of the system in the "x"-direction, it is possible to make the ansatz

:psileft(x,z,t ight)=e^{ialphaleft(x-ct ight)}Psileft(z ight),,

where alpha, is a spatial wavenumber. Thus, the problem reduces to solving the equation

:left(D^2-alpha^2 ight)Psi_j=0,,,, D=frac{d}{dz},,,, j=L,G.,

The domain of the problem is the following: the fluid with label `L' livesin the region -infty, while the fluid with the label `G' livesin the upper half-plane 0leq z. To specify the solution fully, it is necessary to fix conditions at the boundaries and interface. This determines the wave speed "c", which in turn determiens the stabilty properties of the system.

The first of these conditions is provided by details at the boundary. Theperturbation velocities w'_i, should satisfy a no-flux condition, so thatfluid does not leak out at the boundaries z=pminfty., Thus, w_L'=0,on z=-infty,, and w_G'=0, on z=infty,. In terms of the streamfunction, this is

:Psi_Lleft(-infty ight)=0,qquad Psi_Gleft(infty ight)=0.,

The other three conditions are provided by details at the interface z=etaleft(x,t ight),.

"Continuity of vertical velocity:" At z=eta, the vertical velocities match, w'_L=w'_G,. Using the streamfunction representation, this gives

:Psi_Lleft(eta ight)=Psi_Gleft(eta ight).,

Expanding about z=0, gives

:Psi_Lleft(0 ight)=Psi_Gleft(0 ight)+ ext{H.O.T.},,

where H.O.T. means `higher-order terms'. This equation is the required interfacialcondition.

"The free-surface condition:" At the free surface z=etaleft(x,t ight),, the kinematic condition holds:

:frac{partialeta}{partial t}+u'frac{partialeta}{partial x}=w'left(eta ight).,

Linearizing, this is simply

:frac{partialeta}{partial t}=w'left(0 ight),,

where the velocity w'left(eta ight), is linearized on to the surfacez=0,. Using the normal-mode and streamfunction representations, this condition is c eta=Psi,, the second interfacial condition.

"Pressure relation across the interface:" For the case with surface tension, the pressure difference over the interface at z=eta is given by the Young–Laplace equation:

:p_Gleft(z=eta ight)-p_Lleft(z=eta ight)=sigmakappa,,

where "σ" is the surface tension and "κ" is the curvature of the interface, which in a linear approximation is

:kappa= abla^2eta=eta_{xx}.,


:p_Gleft(z=eta ight)-p_Lleft(z=eta ight)=sigmaeta_{xx}.,

However, this condition refers to the total pressure (base+perturbed),thus

:left [P_Gleft(eta ight)+p'_Gleft(0 ight) ight] -left [P_Lleft(eta ight)+p'_Lleft(0 ight) ight] =sigmaeta_{xx}.,

(As usual, The perturbed quantities can be linearized onto the surface "z=0".) Using hydrostatic balance, in the form

:P_L=- ho_L g z+p_0,qquad P_G=- ho_G gz +p_0,,

this becomes

:p'_G-p'_L=getaleft( ho_G- ho_L ight)+sigmaeta_{xx},qquad ext{on }z=0.,

The perturbed pressures are evaluated in terms of streamfunctions, using the horizontal momentum equation of the linearised Euler equations for the perturbations, frac{partial u_i'}{partial t} = - frac{1}{ ho_i}frac{p_i'}{partial x}, with i=L,G,, to yield

:p_i'= ho_i c DPsi_i,qquad i=L,G.,

Putting this last equation and the jump condition together,

:cleft( ho_G DPsi_G- ho_L DPsi_L ight)=getaleft( ho_G- ho_L ight)+sigmaeta_{xx}.,

Substituting the second interfacial condition ceta=Psi, and using the normal-mode representation, this relationbecomes

:c^2left( ho_G DPsi_G- ho_L DPsi_L ight)=gPsileft( ho_G- ho_L ight)-sigmaalpha^2Psi,,

where there is no need to label Psi, (only its derivatives) because Psi_L=Psi_G,at z=0.,


Now that the model of stratified flow has b een set up, the solution is at hand. The streamfunction equation left(D^2-alpha^2 ight)Psi_i=0,, with the boundary conditions Psileft(pminfty ight), has the solution

:Psi_L=A_L e^{alpha z},qquad Psi_G = A_G e^{-alpha z}.,

The first interfacial condition states that Psi_L=Psi_G, at z=0,, whichforces A_L=A_G=A., The third interfacial condition states that

:c^2left( ho_G DPsi_G- ho_L DPsi_L ight)=gPsileft( ho_G- ho_L ight)+sigmaalpha^2.,

Plugging the solution into this equation gives the relation

:Ac^2alphaleft(- ho_G- ho_L ight)=Agleft( ho_G- ho_L ight).,

The "A" cancels from both sides and we are left with

:c^2=frac{g}{alpha}frac{ ho_L- ho_G}{ ho_L+ ho_G}+frac{sigmaalpha}{ ho_L+ ho_G}.,

To understand the implications of this result in full, it is helpful to consider the case of zero surface tension. Then,

:c^2=frac{g}{alpha}frac{ ho_L- ho_G}{ ho_L+ ho_G},qquad sigma=0,,

and clearly

* If ho_G< ho_L,, c^2>0, and "c" is real. This happens when thelighter fluid sits on top;
* If ho_G> ho_L,, c^2<0, and "c" is purely imaginary. This happenswhen the heavier fluid sits on top.

Now, when the heavier fluid sits on top, c^2<0,, and

:c=pm i sqrt{frac{gmathcal{A{alpha,qquad mathcal{A}=frac{ ho_G- ho_L}{ ho_G+ ho_L},,

where mathcal{A}, is the Atwood number. By taking the positive solution,we see that the solution has the form

:Psileft(x,z,t ight)=Ae^{-alpha|zexpleft [ialphaleft(x-ct ight) ight] =Aexpleft(alphasqrt{frac{g ilde{mathcal{A}{alphat ight)expleft(ialphax-alpha|z| ight),

and this is associated to the interface position "η" by: ceta=Psi., Now define B=A/c.,

url=http://math.lanl.gov/Research/Highlights/amrmhd.shtml | title=Parallel AMR Code for Compressible MHD or HD Equations | author=Li, Shengtai and Hui Li | publisher=Los Alamos National Laboratory | accessdate=2006-09-05]

The time evolution of the free interface elevation z = eta(x,t),, initially at eta(x,0)=Releft{B,expleft(ialpha x ight) ight},, is given by:

:eta=Releft{B,expleft(sqrt{mathcal{A}galpha},t ight)expleft(ialpha x ight) ight},

which grows exponentially in time. Here "B" is the amplitude of the initial perturbation, and Releft{cdot ight}, denotes the real part of the complex valued expression between brackets.

In general, the condition for linear instability is that the imaginary part of the "wave speed" "c" be positive. Finally, restoring the surface tension makes "c"2 less negative and is therefore stabilizing. Indeed, there is a range of short waves for which the surface tension stabilizes the system and prevents the instability forming.

Late-time behaviour

The analysis of the previous section breaks down when the amplitude of the perturbation is large. Then, as in the figure, numerical simulation of the full problem is required to describe the system.

ee also

*Richtmyer-Meshkov instability
*Kelvin–Helmholtz instability
*Mushroom cloud
*Plateau-Rayleigh instability
*Salt fingering
*Kármán vortex street



Original research papers

*cite journal| author=Rayleigh, Lord (John William Strutt) | authorlink=John Strutt, 3rd Baron Rayleigh | title=Investigation of the character of the equilibrium of an incompressible heavy fluid of variable density | journal=Proceedings of the London Mathematical Society | volume=14 | pages=170–177 | year=1883 |doi=10.1112/plms/s1-14.1.170 (Original paper is available at: https://www.irphe.univ-mrs.fr/~clanet/otherpaperfile/articles/Rayleigh/rayleigh1883.pdf .)
*cite journal| author=Taylor, Sir Geoffrey Ingram | authorlink=Geoffrey Ingram Taylor | title=The instability of liquid surfaces when accelerated in a direction perpendicular to their planes | journal=Proceedings of the Royal Society of London. Series A, Mathematical and Physical Sciences | volume=201 | issue=1065 | pages=192–196 | year=1950 | doi=10.1098/rspa.1950.0052


*cite book| author=Chandrasekhar, Subrahmanyan | authorlink=Subrahmanyan Chandrasekhar | title=Hydrodynamic and Hydromagnetic Stability | publisher=Dover Publications | year=1981 | isbn=978-0486640716
*cite book| title=Introduction to hydrodynamic stability | first=P. G. | last=Drazin | publisher=Cambridge University Press | year=2002 | isbn=0 521 00965 0 xvii+238 pages.
*cite book | author= Drazin, P. G. | coauthors=Reid, W. H. | title= Hydrodynamic stability | date=2004 | publisher=Cambridge University Press | location=Cambridge | isbn=0-521-52541-1 |edition=2nd edition 626 pages.

External links

* [http://acg.media.mit.edu/people/fry/mixing/ Java demonstration of the RT instability in fluids]
* [http://www.enseeiht.fr/hmf/travaux/CD0001/travaux/optmfn/hi/01pa/hyb72/rt/rt.htm Actual images and videos of RT fingers]
* [http://web.arizona.edu/~fluidlab/ Experiments on Rayleigh-Taylor experiments at the University of Arizona]

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