This article will be permanently flagged as inappropriate and made unaccessible to everyone. Are you certain this article is inappropriate? Excessive Violence Sexual Content Political / Social
Email Address:
Article Id: WHEBN0000164313 Reproduction Date:
In fluid dynamics, gravity waves are waves generated in a fluid medium or at the interface between two media when the force of gravity or buoyancy tries to restore equilibrium. An example of such an interface is that between the atmosphere and the ocean, which gives rise to wind waves.
When a fluid element is displaced on an interface or internally to a region with a different density, gravity will try to restore it toward equilibrium, resulting in an oscillation about the equilibrium state or wave orbit.^{[1]} Gravity waves on an air–sea interface of the ocean are called surface gravity waves or surface waves, while gravity waves that are within the body of the water (such as between parts of different densities) are called internal waves. Wind-generated waves on the water surface are examples of gravity waves, as are tsunamis and ocean tides.
Wind-generated gravity waves on the free surface of the Earth's ponds, lakes, seas and oceans have a period of between 0.3 and 30 seconds (3 Hz to 0.03 Hz). Shorter waves are also affected by surface tension and are called gravity–capillary waves and (if hardly influenced by gravity) capillary waves. Alternatively, so-called infragravity waves, which are due to subharmonic nonlinear wave interaction with the wind waves, have periods longer than the accompanying wind-generated waves.^{[2]}
In the Earth's atmosphere, gravity waves are a mechanism for the transfer of momentum from the troposphere to the stratosphere. Gravity waves are generated in the troposphere by frontal systems or by airflow over mountains. At first, waves propagate through the atmosphere without appreciable change in mean velocity. But as the waves reach more rarefied (thin) air at higher altitudes, their amplitude increases, and nonlinear effects cause the waves to break, transferring their momentum to the mean flow.
This process plays a key role in studying the dynamics of the middle atmosphere.
The clouds in gravity waves can look like altostratus undulatus clouds, and are sometimes confused with them, but the formation mechanism is different.
The phase velocity \scriptstyle c of a linear gravity wave with wavenumber \scriptstyle k is given by the formula
c=\sqrt{\frac{g}{k}},
where g is the acceleration due to gravity. When surface tension is important, this is modified to
c=\sqrt{\frac{g}{k}+\frac{\sigma k}{\rho}},
where σ is the surface tension coefficient and ρ is the density.
The gravity wave represents a perturbation around a stationary state, in which there is no velocity. Thus, the perturbation introduced to the system is described by a velocity field of infinitesimally small amplitude, \scriptstyle (u'(x,z,t),w'(x,z,t)). Because the fluid is assumed incompressible, this velocity field has the streamfunction representation
where the subscripts indicate partial derivatives. In this derivation it suffices to work in two dimensions \scriptstyle \left(x,z\right), where gravity points in the negative z-direction. Next, in an initially stationary incompressible fluid, there is no vorticity, and the fluid stays irrotational, hence \scriptstyle\nabla\times\textbf{u}'=0.\, In the streamfunction representation, \scriptstyle\nabla^2\psi=0.\, Next, because of the translational invariance of the system in the x-direction, it is possible to make the ansatz
where k is a spatial wavenumber. Thus, the problem reduces to solving the equation
We work in a sea of infinite depth, so the boundary condition is at \scriptstyle z=-\infty. The undisturbed surface is at \scriptstyle z=0, and the disturbed or wavy surface is at \scriptstyle z=\eta, where \scriptstyle\eta is small in magnitude. If no fluid is to leak out of the bottom, we must have the condition
Hence, \scriptstyle\Psi=Ae^{k z} on \scriptstyle z\in\left(-\infty,\eta\right), where A and the wave speed c are constants to be determined from conditions at the interface.
The free-surface condition: At the free surface \scriptstyle z=\eta\left(x,t\right)\,, the kinematic condition holds:
Linearizing, this is simply
where the velocity \scriptstyle w'\left(\eta\right)\, is linearized on to the surface \scriptstyle z=0.\, Using the normal-mode and streamfunction representations, this condition is \scriptstyle 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 \scriptstyle z=\eta is given by the Young–Laplace equation:
where σ is the surface tension and κ is the curvature of the interface, which in a linear approximation is
Thus,
However, this condition refers to the total pressure (base+perturbed), thus
(As usual, The perturbed quantities can be linearized onto the surface z=0.) Using hydrostatic balance, in the form \scriptstyle P=-\rho g z+\text{Const.},
this becomes
The perturbed pressures are evaluated in terms of streamfunctions, using the horizontal momentum equation of the linearised Euler equations for the perturbations,
to yield \scriptstyle p'=\rho c D\Psi.
Putting this last equation and the jump condition together,
Substituting the second interfacial condition \scriptstyle c\eta=\Psi\, and using the normal-mode representation, this relation becomes \scriptstyle c^2\rho D\Psi=g\Psi\rho+\sigma k^2\Psi.
Using the solution \scriptstyle \Psi=e^{k z}, this gives
c=\sqrt{\frac{g}{k}+\frac{\sigma k}{\rho}}.
Since \scriptstyle c=\omega/k is the phase speed in terms of the angular frequency \scriptstyle\omega and the wavenumber, the gravity wave angular frequency can be expressed as
\omega=\sqrt{gk}.
The group velocity of a wave (that is, the speed at which a wave packet travels) is given by
c_g=\frac{d\omega}{dk},
and thus for a gravity wave,
c_g=\frac{1}{2}\sqrt{\frac{g}{k}}=\frac{1}{2}c.
The group velocity is one half the phase velocity. A wave in which the group and phase velocities differ is called dispersive.
Gravity waves traveling in shallow water (where the depth is much less than the wavelength), are nondispersive: the phase and group velocities are identical and independent of wavelength and frequency. When the water depth is h,
Wind waves, as their name suggests, are generated by wind transferring energy from the atmosphere to the ocean's surface, and capillary-gravity waves play an essential role in this effect. There are two distinct mechanisms involved, called after their proponents, Phillips and Miles.
In the work of Phillips,^{[3]} the ocean surface is imagined to be initially flat (glassy), and a turbulent wind blows over the surface. When a flow is turbulent, one observes a randomly fluctuating velocity field superimposed on a mean flow (contrast with a laminar flow, in which the fluid motion is ordered and smooth). The fluctuating velocity field gives rise to fluctuating stresses (both tangential and normal) that act on the air-water interface. The normal stress, or fluctuating pressure acts as a forcing term (much like pushing a swing introduces a forcing term). If the frequency and wavenumber \scriptstyle\left(\omega,k\right) of this forcing term match a mode of vibration of the capillary-gravity wave (as derived above), then there is a resonance, and the wave grows in amplitude. As with other resonance effects, the amplitude of this wave grows linearly with time.
The air-water interface is now endowed with a surface roughness due to the capillary-gravity waves, and a second phase of wave growth takes place. A wave established on the surface either spontaneously as described above, or in laboratory conditions, interacts with the turbulent mean flow in a manner described by Miles.^{[4]} This is the so-called critical-layer mechanism. A critical layer forms at a height where the wave speed c equals the mean turbulent flow U. As the flow is turbulent, its mean profile is logarithmic, and its second derivative is thus negative. This is precisely the condition for the mean flow to impart its energy to the interface through the critical layer. This supply of energy to the interface is destabilizing and causes the amplitude of the wave on the interface to grow in time. As in other examples of linear instability, the growth rate of the disturbance in this phase is exponential in time.
This Miles–Phillips Mechanism process can continue until an equilibrium is reached, or until the wind stops transferring energy to the waves (i.e., blowing them along) or when they run out of ocean distance, also known as fetch length.
Earth, Solar System, Antarctica, Atlantic Ocean, Physical oceanography
2011 Tōhoku earthquake and tsunami, Thucydides, Thailand, Hawaii, Unesco
Ocean, Atlantic Ocean, Oceanography, Marine geology, Geology
Mass, Velocity, Energy, Time, Acceleration
Jupiter, Mars, Venus, Earth, Nitrogen
Wind wave, Physical oceanography, Antarctica, Swell (ocean), Tsunami
Physical oceanography, Ocean, Wind, Tsunami, Wave power
Sound, Gravity wave, Corona, Wave, Plasma wave
Pennsylvania, Meteorology, Temperature, Wind, Aviation accidents and incidents
Structure, Tsunami, Earthquake engineering, Gravity wave, Earthquake