View source for Kuramoto-Sivashinsky equation

''Sivashinsky–Kuramoto equation, KS equation''

The Kuramoto–Sivashinsky equation in one space dimension, in  "derivative"  form

<table class="eq" style="width:100%;"> <tr><td valign="top" style="width:94%;text-align:center;"><img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k1300701.png" /></td> <td valign="top" style="width:5%;text-align:right;">(a1)</td></tr></table>

or in  "integral"  form

<table class="eq" style="width:100%;"> <tr><td valign="top" style="width:94%;text-align:center;"><img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k1300702.png" /></td> </tr></table>

where <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k1300703.png" />, has attracted a great deal of interest as a model for complex spatio-temporal dynamics in spatially extended systems, and as a paradigm for finite-dimensional dynamics in a partial differential equation.

The Kuramoto–Sivashinsky equation (with various alternative scalings for <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k1300704.png" />, <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k1300705.png" /> or <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k1300706.png" />, which can be reduced to the form (a1)) has been independently derived in the context of several extended physical systems driven far from equilibrium by intrinsic instabilities, including instabilities of dissipative trapped ion modes in plasmas [[#References|[a21]]], [[#References|[a5]]], instabilities in laminar flame fronts [[#References|[a31]]], phase dynamics in reaction-diffusion systems [[#References|[a19]]], and fluctuations in fluid films on inclines [[#References|[a30]]]. Indeed, (a1) generically describes the dynamics near long-wave-length primary instabilities in the presence of appropriate (translational, parity and Galilean) symmetries [[#References|[a24]]].

The <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k1300707.png" /> term in (a1) is responsible for an instability at large scales; the dissipative <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k1300708.png" /> term provides damping at small scales; and the non-linear term <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k1300709.png" /> (which has the same form as that in the Burgers or one-dimensional [[Navier–Stokes equations|Navier–Stokes equations]]) stabilizes by transferring energy between large and small scales. This is readily apparent in Fourier space, where one may write (a1) with periodic boundary conditions as

<table class="eq" style="width:100%;"> <tr><td valign="top" style="width:94%;text-align:center;"><img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007010.png" /></td> <td valign="top" style="width:5%;text-align:right;">(a2)</td></tr></table>

where <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007011.png" />, <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007012.png" />, <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007013.png" />, <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007014.png" />, <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007015.png" />. The zero solution is linearly unstable to modes with <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007016.png" />; these modes, whose number is proportional to the [[Bifurcation|bifurcation]] parameter <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007017.png" />, are coupled to each other and to damped modes at <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007018.png" /> through the non-linear term.

As <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007019.png" /> increases beyond <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007020.png" />, therefore, the zero solution destabilizes, initially to a single-humped stationary  "cellular"  state, which then in turn becomes unstable through a complex hierarchy of bifurcations including multi-modal stationary, oscillatory and chaotic solutions, which have been characterized in detail [[#References|[a15]]], [[#References|[a13]]], [[#References|[a17]]]. Note that as suggested by the presence of chaotic solutions and by a Painlevé analysis [[#References|[a7]]] (cf. also [[Painlevé test|Painlevé test]]), the Kuramoto–Sivashinsky equation is non-integrable, and no explicit general analytic solutions exist. A striking feature of the bifurcation behaviour in this partial differential equation, especially for relatively small <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007021.png" />, is the apparent low-dimensionality of the dynamics, and the similarity of the observed bifurcations to those found in (low) finite-dimensional systems. Motivated by this observation, extensive analytical study of the solutions has shown that the Kuramoto–Sivashinsky equation is rigorously equivalent to a finite-dimensional dynamical system (for an overview of analytical results in an appropriate functional setting, see [[#References|[a32]]]).

==Analytical results and finite-dimensionality of dynamics.==
Specifically, a significant feature of the Kuramoto–Sivashinsky dynamics is its dissipativity (cf. also [[Dissipative system|Dissipative system]]): solutions are attracted to an absorbing ball, with <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007022.png" />-dependent radius, in <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007023.png" /> and higher Sobolev spaces ([[#References|[a26]]] for odd initial data, [[#References|[a2]]], [[#References|[a12]]] for general periodic solutions; cf. also [[Sobolev space|Sobolev space]]). The strong smoothing properties of the linear operator in fact imply boundedness in the Gevrey norm (cf. [[Gevrey class|Gevrey class]]) and thus space-analyticity of solutions of (a1) [[#References|[a3]]], as well as time-analyticity [[#References|[a16]]].

The dissipativity of the dynamics has been used to show [[#References|[a26]]] that the system (a1) has a finite number of determining modes, and a compact global attractor with finite fractal and [[Hausdorff dimension|Hausdorff dimension]]. While the attractor can have very complex structure, a stronger result is the existence of a finite-dimensional inertial manifold, which exponentially absorbs solutions and contains the global attractor [[#References|[a10]]], [[#References|[a4]]]. On restricting the partial differential equation to the inertial manifold, one obtains a system of ordinary differential equations, the inertial form, which completely describes the long-time dynamics; thus, the Kuramoto–Sivashinsky equation is rigorously equivalent to a finite-dimensional [[Dynamical system|dynamical system]]. The existence of the inertial manifold does not provide an explicit construction, however, so various approximation schemes have been introduced; for instance, one can construct approximate inertial manifolds so that all trajectories of the Kuramoto–Sivashinsky equation approach the approximate inertial manifold at an exponential rate [[#References|[a16]]].

==Bifurcations and elementary solutions.==
The cellular or  "roll"  solutions [[#References|[a11]]] form the backbone to the spatial structure of solutions of (a1) (with periodic boundary conditions) observed as <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007024.png" /> increases: the <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007025.png" />-cell state consists of solutions with periodicity <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007026.png" /> which lie on the branch bifurcating from the trivial solution at <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007027.png" />, and have rapidly decreasing basin of attraction for increasing <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007028.png" /> [[#References|[a9]]]. Other solutions observed numerically for increasing <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007029.png" />, and in some cases accounted for analytically, include other families of stationary states, time-periodic standing and travelling waves, quasi-periodic modulated travelling waves, and heteroclinic cycles [[#References|[a1]]], [[#References|[a17]]]. There are also windows in which strange attractors with positive Lyapunov exponents (cf. [[Lyapunov characteristic exponent|Lyapunov characteristic exponent]]) are observed, together with more complex dynamical phenomena associated with chaotic dynamics, including period doubling cascades, Shil'nikov connections and crises of chaos.

==Spatio-temporal chaos.==
As <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007030.png" /> increases and one passes through an increasingly intricate bifurcation sequence of ordered and chaotic states, eventually one reaches a state of persistent dynamical disorder for (almost) all sufficiently large <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007031.png" /> [[#References|[a13]]] (see Fig.a1), and there is strong numerical evidence that the  "simple"  solutions destabilize to an (apparently unique) spatio-temporally chaotic attractor (see [[#References|[a8]]] for a review of spatio-temporal pattern formation).

<img style="border:1px solid;" src="https://www.encyclopediaofmath.org/legacyimages/common_img/k130070a.gif" />

Figure: k130070a

A solution <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007032.png" /> of the Kuramoto–Sivashinsky equation (a1)on the spatio-temporally chaotic attractor, for <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007033.png" />, and covering <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007034.png" /> time units separated by <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007035.png" />

This regime of  "weak"  or  "phase"  turbulence [[#References|[a23]]] is distinct from the  "strong"  turbulence exhibited in, for instance, the [[Navier–Stokes equations|Navier–Stokes equations]] for fluids, in that there are no major excursions from space or time averages. While the individual solutions bifurcating from the zero solution break the translational, parity and Galilean symmetries of (a1), the spatio-temporally chaotic state displays  "re-emergent order" , in that the symmetries are restored in a statistically averaged sense.

Numerical evidence indicates that the spatio-temporally chaotic state is characterized by a finite density of positive Lyapunov exponents, that is, the Lyapunov dimension of the attractor is proportional to <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007036.png" /> [[#References|[a22]]]. In fact, in general there appears to be  "extensive chaos"  for sufficiently large <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007037.png" />: that is, due to rapid decay of spatial correlations [[#References|[a33]]] local dynamics are asymptotically independent of system size <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007038.png" />, extensive quantities such as the energy (square of the <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007039.png" /> norm) scale with <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007040.png" />, and one can hope to study the thermodynamic limit, interpreting the large system as being composed of weakly interacting smaller subsystems.

However, this picture is as yet by no means well-established, and even relatively  "simple"  analytical results on intensive properties which might seem rigorously provable, have remained elusive at the time of this writing (2000). For example, the known analytical and numerical solutions all appear to have uniformly bounded <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007041.png" />, that is, the <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007042.png" /> norm <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007043.png" /> is bounded independent of <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007044.png" />; this would imply the existence of a finite energy density, or that the <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007045.png" /> norm

<table class="eq" style="width:100%;"> <tr><td valign="top" style="width:94%;text-align:center;"><img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007046.png" /></td> </tr></table>

is proportional to <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007047.png" />. While a uniform bound on <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007048.png" /> is known for stationary solutions [[#References|[a25]]] and solutions near these on the attractor, currently (2000) the best known general bound for <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007049.png" /> is <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007050.png" /> [[#References|[a2]]]. Similarly, based on extensive numerical evidence, it has been conjectured [[#References|[a2]]], [[#References|[a27]]], [[#References|[a26]]] that the attractor and inertial manifold dimensions scale linearly with <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007051.png" />, or with the number of linearly unstable Fourier modes, while the radius of the strip of space-analyticity is <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007052.png" />-independent [[#References|[a3]]]; but the best known rigorous bounds for the Kuramoto–Sivashinsky equation do not yet approach this thermodynamic limit.

The dynamics on the spatio-temporally complex attractor for large <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007053.png" /> are best understood in the light of the characteristic shape of the normalized (time-averaged) power spectrum <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007054.png" />, which appears to be independent of <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007055.png" /> in the disordered regime, consistent with a finite energy density [[#References|[a27]]], [[#References|[a28]]] (see Fig.a2).

The power spectrum reveals three distinct regimes of the dynamics, whose dynamical significance is corroborated by other evidence including numerical experiments in which different modes are eliminated or forced [[#References|[a33]]]: The exponential tail in <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007056.png" /> is due to strong dissipation at small scales (high <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007057.png" />), corresponding to the exponential decay of Fourier modes of an analytic function; these modes are strongly damped and essentially irrelevant for the qualitative dynamics. The active scales for <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007058.png" /> have distinctly non-Gaussian distributions and contain most of the energy, with a pronounced peak near <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007059.png" />, the most linearly unstable mode; the localized dynamics at these scales, which may be interpreted as cell creation and annihilation events [[#References|[a6]]], are essential to the spatio-temporal disorder.

<img style="border:1px solid;" src="https://www.encyclopediaofmath.org/legacyimages/common_img/k130070b.gif" />

Figure: k130070b

Rescaled power spectrum <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007060.png" />, for <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007061.png" /> and <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007062.png" />

In the large scale region, there is a shoulder in <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007063.png" /> which flattens as <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007064.png" />, reminiscent of a thermodynamic regime with equipartition of energy. These scales exhibit Gaussian statistics and appear to act as a  "heat bath" , providing the background excitation needed to maintain the spatio-temporal disorder [[#References|[a33]]]. There has been considerable effort devoted towards understanding the effective stochastic dynamics at large length and time scales [[#References|[a35]]], [[#References|[a29]]], [[#References|[a20]]], [[#References|[a6]]]. The (deterministic) chaotic dynamics at active and small scales simulate the effect of random forcing on the largest scales, and act to renormalize the viscosity, so that the scaling of solutions at large scales appears to be well-described by a noise-driven Burgers equation or, equivalently, the Kardar–Parisi–Zhang equation for kinetic roughening [[#References|[a34]]], [[#References|[a18]]] (see [[#References|[a14]]] for a review).

Numerous investigators have extended the above-mentioned results on the analysis and dynamics of the Kuramoto–Sivashinsky equation in the small-<img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007065.png" /> and large-<img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007066.png" /> regimes, and have studied generalizations to higher space dimensions and non-periodic boundary conditions (including the unbounded system, <img align="absmiddle" border="0" src="https://www.encyclopediaofmath.org/legacyimages/k/k130/k130070/k13007067.png" />), and the effect of additional terms in the partial differential equation.

====References====
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