Inertial wave

Inertial waves, also known as inertial oscillations, are a type of mechanical wave possible in rotating fluids. Unlike surface gravity waves commonly seen at the beach or in the bathtub, inertial waves travel through the bulk of the fluid, not at the surface. Like any other kind of wave, an inertial wave is caused by a restoring force and characterized by its wavelength and frequency. Because the restoring force for inertial waves is the Coriolis force, their wavelengths and frequencies are related in a peculiar way. Inertial waves are transverse. Most commonly they are observed in atmospheres, oceans, lakes, and laboratory experiments. Rossby waves, geostrophic currents, and geostrophic winds are examples of inertial waves. Inertial waves are also likely to exist in the core of the Earth.

Restoring force

To understand the idea of a restoring force, imagine a guitar string. In , the string is taut and straight, held stationary between its ends. Plucking the string moves it away from this equilibrium position. The tension in the string immediately pulls it back toward equilibrium, but soon overshoots, so that the string bows in the opposite direction. Next, tension again pulls the string back toward equilibrium, but again overshoots, and the cycle continues until the string finally comes to rest. Since tension restores the string to equilibrium (overshooting many times along the way), it is called the restoring force. Without it, the string would not vibrate, and no wave could exist.

Likewise, the open ocean is in equilibrium when it is level and at rest. If something (like wind) causes part of the ocean to rise and form a crest, the crest is immediately pulled back toward equilibrium by gravity. Soon gravity overshoots, and the crest becomes a trough, displacing water and forming other crests nearby. They, in turn, are pulled back toward equilibrium by gravity, and the cycle continues. So gravity is the restoring force for wind waves on the open ocean, often called gravity waves.

Inertial waves are restored to equilibrium by the Coriolis force, a result of rotation. To be precise, the Coriolis force arises (along with the centrifugal force) in a rotating frame to account for the fact that such a frame is always accelerating. Inertial waves, therefore, cannot exist without rotation. More complicated than tension on a string, the Coriolis force acts at a 90° angle to the direction of motion, and its strength depends on the rotation rate of the fluid. These two properties lead to the peculiar characteristics of inertial waves.

Characteristics

Inertial waves are possible only when a fluid is rotating, and exist in the bulk of the fluid, not at its surface. Like light waves, inertial waves are transverse, which means that their vibrations occur perpendicular to the direction of wave travel. (The opposite of a transverse wave is a longitudinal wave, where the vibrations are in the same direction as the wave travel. Sound waves, for example, are longitudinal.) One peculiar geometrical characteristic of inertial waves is that their phase velocity, which tells about the movement of the "crests" and "troughs" of the wave, is "perpendicular" to their group velocity, which tells about the propagation of energy.

Whereas a sound wave or an electromagnetic wave of any frequency is possible, inertial waves can exist only over the range of frequencies from zero to twice the rotation rate of the fluid. Moreover, the frequency of the wave is determined by its direction of travel. Waves traveling perpendicular to the axis of rotation have zero frequency and are sometimes called the geostrophic modes. Waves traveling parallel to the axis have maximum frequency (twice the rotation rate), and waves at intermediate angles have intermediate frequencies. In free space, an inertial wave can exist at "any" frequency between 0 and twice the rotation rate. A closed container, however, can impose restrictions on the possible frequencies of inertial waves, as it can for any kind of wave. Inertial waves in a closed container are often called inertial modes. In a sphere, for example, the inertial modes are forced to take on discrete frequencies, leaving gaps where no modes can exist.

Examples of inertial waves

Any kind of fluid can support inertial waves: water, oil, liquid metals, air, and other gases. Inertial waves are observed most commonly in planetary atmospheres (Rossby waves, geostrophic winds) and in oceans and lakes (geostropic currents), where they are responsible for much of the mixing that takes place. Inertial waves affected by the slope of the ocean floor are often called Rossby waves. Inertial waves can be observed in laboratory experiments or in industrial flows where a fluid is rotating. Inertial waves are also likely to exist in the liquid outer core of the Earth, and at least one group [http://www.nature.com/nature/journal/v325/n6103/abs/325421a0.html] has claimed evidence of them. Similarly, inertial waves are likely in rotating astronomical flows like accretion disks, planetary rings, and galaxies.

Mathematical description

Fluid flow is governed by the momentum equation (often called the Navier-Stokes equation) which is essentially a statement of Newton's second law for the fluid. The velocity $vec\{u\}$ in a fluid with viscosity $u$ under pressure $P$ and rotating at rate $Omega$ changes over time $t$ according to

: $frac\{partial\; vec\{u\{partial\; t\}+\; (vec\{u\}\; cdot\; vec\{\; abla\})\; vec\{u\}=\; -\; frac\{1\}\{\; ho\}\; vec\{\; abla\}P+\; u\; abla^2\; vec\{u\}-\; 2vec\{Omega\}\; imes\; vec\{u\}.$

To be precise, $vec\{u\}$ is the velocity of the fluid as observed in the rotating frame of reference. Since a rotating frame of reference is always accelerating (a so-called non-inertial frame), two additional forces (as mentioned above) must be introduced: the centripetal force and the Coriolis force. In the equation above, the centripetal force is actually part of the generalized pressure $P$, that is, $P$ is related to the usual pressure $p$, depending on the distance from the rotation axis $r$, by

: $P\; =\; p\; +\; ho\; r^2\; Omega^2.$

The last term on the right side of the momentum equation is the Coriolis term. The first term on the right accounts for pressure, and the second accounts for viscous diffusion.

In the case where the rotation rate is large, the Coriolis force and the centripetal force become large compared to the other terms. Being small in comparison, diffusion and the "convective derivative" (second term on the left) can be left out. Taking a curl of both sides and applying a few vector identities, the result is

: $frac\{partial\}\{partial\; t\}\; abla\; imes\; vec\{u\}\; =\; 2\; (\; vec\{Omega\}\; cdot\; vec\{\; abla\}\; )\; vec\{u\}.$

Solutions to this equation are waves that satisfy two conditions. First, if $vec\{k\}$ is the wave vector,

: $vec\{u\}\; cdot\; vec\{k\}\; =\; 0,$

that is, the waves must be transverse, as mentioned above. Second, solutions are required to have a frequency $omega$ that satisfies the dispersion relation

:$omega\; =\; 2\; hat\{k\}\; cdot\; vec\{Omega\}\; =\; 2\; Omega\; cos\{\; heta\},$

where $heta$ is the angle between the axis of roation and the direction of the wave. These particular solutions are known as inertial waves.

The dispersion relation looks much like the Coriolis term in the momentum equation--notice the rotation rate and the factor of two. It immediately implies the range of possible frequencies for inertial waves, as well as the dependence of their frequency on their direction.

Further reading

*cite journal | last=Aldridge | first=K. D. | coauthors=I. Lumb | title=Inertial waves identified in the Earth's fluid outer core | journal=Nature | volume=325 | pages=421–423 | date=1987 | doi=10.1038/325421a0

*cite book | last=Greenspan | first=H. P. | title=The Theory of Rotating Fluids | publisher=Cambridge University Press | year=1969

*cite book | last=Landau | first=L. D. | coauthors=E. M. Lifschitz | title=Fluid Mechanics, Second Edition | publisher=Elsevier | location=New York | year=1987 | id=ISBN 0-7506-2767-0