# Difference between revisions of "Capillary waves"

## Thermal capillary waves

Thermal capillary waves are oscillations of an interface which are thermal in origin. These take place at the molecular level, where only the contribution due to surface tension is relevant. Capillary wave theory is a classic account of how thermal fluctuations distort an interface (Ref. 1). It starts from some intrinsic surface that is distorted. In the Monge representation, the surface is given as $z=h(x,y)$. An increase in area of the surface causes a proportional increase of energy: $E_\mathrm{st}= \sigma \iint dx\, dy\ \sqrt{1+\left( \frac{dh}{dx} \right)^2+\left( \frac{dh}{dy} \right)^2} -1$

for small values of the derivatives (surfaces not too rough): $E_\mathrm{st} \approx \frac{\sigma}{2} \iint dx\, dy\ \left[ \left( \frac{dh}{dx} \right)^2+\left( \frac{dh}{dy} \right)^2 \right].$

A Fourier analysis treatment begins by writing the intrinsic surface as an infinite sum of normal modes: $h(x,y)= \sum_\vec{q} a_\vec{q} e^{i\vec{q}\vec{r}}.$

Since normal modes are orthogonal, the energy is easily expressible as a sum of terms $\propto q^2 |a_\vec{q}|^2$. Each term of the sum is quadratic in the amplitude; hence equipartition holds, according to standard classical statistical mechanics, and the mean energy of each mode will be $k_B T/2$. Surprisingly, this result leads to a divergent surface (the width of the interface is bound to diverge with its area) (Ref 2). This divergence is nevertheless very mild; even for displacements on the order of meters, the deviation of the surface is comparable to the size of the molecules. Moreover, the introduction of an external field removes this divergence: the action of gravity is sufficient to keep the width fluctuation on the order of one molecular diameter for areas larger than about 1 mm2 (Ref. 2). The action of gravity is taken into account by integrating the potential energy density due to gravity, $\rho g z$ from a reference height to the position of the surface, $z=h(x,y)$: $E_\mathrm{g}= \iint dx\, dy\, \int_0^h dz \rho g z = \frac{\rho g}{2} \int dx\, dy\, h^2.$

(For simplicity, one neglects the density of the gas above, which is often acceptable; otherwise, instead of the density the difference in densities appears).

Recently, a procedure has been proposed to obtain a molecular intrinsic surface from simulation data (Ref. 3), the intrinsic sampling method. The density profiles obtained from this surface are, in general, quite different from the usual mean density profiles.

## Gravity-capillary waves

These are ordinary waves excited in an interface, such as ripples on a water surface. Their dispersion relation reads, for waves on the interface between two fluids of infinite depth: $\omega^2=\frac{\rho-\rho'}{\rho+\rho'}gk+\frac{\sigma}{\rho+\rho'}k^3,$

where $\omega$ is the angular frequency, $g$ the acceleration due to gravity, $\sigma$ the surface tension, $\rho$ and $\rho^'$ the mass density of the two fluids ( $\rho > \rho^'$) and $k$ the is wavenumber.

### Derivation

This is a sketch of the derivation of the general dispersion relation, see Ref. 4 for a more detailed description. The problem is unfortunately a bit complex. As Richard Feynman put it (Ref. 6):

...[water waves], which are easily seen by everyone and which are used as an example of waves in elementary courses... are the worst possible example... they have all the complications that waves can have

#### Defining the problem

Three contributions to the energy are involved: the surface tension, gravity, and hydrodynamics. The parts due to surface tension (again the derivatives are taken to be small) and gravity are exactly as above. The new contribution involves the kinetic energy of the fluid: $T= \frac{\rho}{2} \iint dx\, dy\, \int_{-\infty}^h dz v^2,$

where $v$ is the module of the velocity field $\vec{v}$. (Again, we are neglecting the flow of the gas above for simplicity.)

#### Wave solutions

Let us suppose the surface of the liquid is described by a traveling plane wave: $h(x,y,t)=\eta(t)e^{i\vec{q}\vec{r}},$

where $\eta(t)=\exp[i\omega t]$ and $\vec{q}=(q_x,q_y)$ is a two dimensional wave number vector, $\vec{r}=(x,y)$ being the horizontal position. We may take $\vec{q}=(q,0)$ without loss of generality: $h(x,y,t)=\eta(t)e^{i q x}.$

In this case it is easy to perform the integrations involved in the expressions for the energies. The integration over $x$ can taken over a period of oscillation $\lambda=2\pi/q$, then multiplied by the number of oscillations in our very large (in principle, infinite) system: $L_x / \lambda$. The integration over $y$ trivially yields $L_y$. Performing the integrations, keeping in mind that only the real part of complex numbers is to be taken as physical, one finds: $E_\mathrm{g} = \frac{A}{2} \frac{\rho g}{2} \eta^2,$ $E_\mathrm{st} = \frac{A}{2} \frac{\sigma}{2} q^2 \eta^2,$

where $A=L_x\times L_y$ is the area of the system.

To tackle the kinetic energy, suppose the fluid is incompressible and its flow is irrotational (often, sensible approximations) - the flow will then be potential: $\vec{v}=\nabla\psi$, and $\psi$ is a potential (scalar field) which must satisfy Laplace's equation $\nabla^2\psi=0$. If we try try separation of variables with the potential: $\psi(x,y,z,t)=\xi(t) f(z) e^{i q x},$

with some function of time $\xi(t)$, and some function of vertical component (height) $f(z)$. Laplace's equation then requires on the later $f''(z)=-q^2 f(z) .$

This equation can be solved with the proper boundary conditions: first, $\vec{v}$ must vanish well below the surface (in the "deep water" case, which is the one we consider, otherwise a more general relation holds, which is also well known in oceanography). Therefore $f(z) = a \, \exp(|q| z)$,

with some constant $a$. The less trivial condition is the proper matching between $\psi$ and $h$: the potential field must correspond to a velocity field that is adjusted to the movement of the surface: $v_z (z=h) =\partial h/\partial t$.

This means that $\xi(t)=\eta(t)'$, and $f'(z=h) = 1,$

so that $f(z) = \exp( -|q|(h-z))/|q|$.

We may now find $v^2=|\nabla\psi|^2$, which is $2 \exp( -2 |q|(h-z)) (\partial h/\partial t)^2$. Performing the $\int_{-\infty}^h$ integration first we are left with $T=\frac{\rho}{2|q|} \int dx\,dy\, \left( \frac{\partial h}{\partial t} \right)^2 \propto \frac{\rho}{2|q|} \left( \eta' \right)^2,$

where we have dropped a factor of $A/4$ in the last step. The problem is thus specified by just a potential energy involving the square of $\eta(t)$ and a kinetic energy involving the square of its time derivative: a regular harmonic oscillator. Its equation of motion will be $\frac{\rho}{|q|} \eta'' + (\rho g+ \sigma q^2) \eta=0,$

whose oscillatory solution is $\omega^2=g k+\frac{\sigma}{\rho}k^3,$

the same dispersion as above if $\rho'$ is neglected.