In geophysics, dynamo theory proposes a mechanism by which a celestial body such as the Earth or a star generates a magnetic field. The theory describes the process through which a rotating, convecting, and electrically conducting fluid can maintain a magnetic field over astronomical time scales.

History of theory

In 1905, shortly after composing his special relativity paper, Albert Einstein described the origin of the Earth's magnetic field as being one of the great unsolved problems facing modern physicists. Since then, there have been many studies of the geodynamo problem based on historical measurements of the Earth's field.

Walter M. Elsasser, considered a "father" of the presently accepted dynamo theory as an explanation of the Earth's magnetism, proposed that this magnetic field resulted from electric currents induced in the fluid outer core of the Earth. He revealed the history of the Earth's magnetic field through pioneering the study of the magnetic orientation of minerals in rocks.

In order to maintain the magnetic field against ohmic decay (which would occur for the dipole field in 20,000 years) the outer core must be convecting. The convection is likely some combination of thermal and compositional convection. The mantle controls the rate at which heat is extracted from the core. Heat sources include gravitational energy released by the compression of the core, gravitational energy released by the rejection of light elements (probably sulfur, oxygen, or silicon) at the inner core boundary as it grows, latent heat of crystallization at the inner core boundary, and radioactivity of potassium, uranium and thorium.

At the dawn of the 21st century, numerical modeling of the Earth's magnetic field has not been successfully demonstrated, but appears to be in reach. Initial models are focused on field generation by convection in the planet's fluid outer core. It was possible to show the generation of a strong, Earth-like field when the model assumed a uniform core-surface temperature and exceptionally high viscosities for the core fluid. Computations which incorporated more realistic parameter values yielded magnetic fields that were less Earth-like, but also point the way to model refinements which may ultimately lead to an accurate analytic model. Slight variations in the core-surface temperature, in the range of a few millikelvins, result in significant increases in convective flow and produce more realistic magnetic fields.

Formal definition

Dynamo theory describes the process through which a rotating, convecting, and electrically conducting fluid acts to maintain a magnetic field. This theory is used to explain the presence of anomalously long-lived magnetic fields in astrophysical bodies. The conductive fluid in the geodynamo is liquid iron in the outer core, and in the solar dynamo is ionized gas at the tachocline. Dynamo theory of astrophysical bodies uses magnetohydrodynamic equations to investigate how the fluid can continuously regenerate the magnetic field.

It was actually once believed that the dipole, which comprises much of the Earth's magnetic field and is misaligned along the rotation axis by 11.3 degrees, was caused by permanent magnetization of the materials in the earth. This means that dynamo theory was originally used to explain the Sun's magnetic field in its relationship with that of the Earth. However, this theory, which was initially proposed by Joseph Larmor in 1919, has been modified due to extensive studies of magnetic secular variation, paleomagnetism (including polarity reversals), seismology, and the solar system's abundance of elements. Also, the application of the theories of Carl Friedrich Gauss to magnetic observations showed that Earth's magnetic field had an internal, rather than external, origin.

There are three requisites for a dynamo to operate:

An electrically conductive fluid medium

Kinetic energy provided by planetary rotation

An internal energy source to drive convective motions within the fluid.

In the case of the Earth, the magnetic field is induced and constantly maintained by the convection of liquid iron in the outer core. A requirement for the induction of field is a rotating fluid. Rotation in the outer core is supplied by the Coriolis effect caused by the rotation of the Earth. The coriolis force tends to organize fluid motions and electric currents into columns (also see Taylor columns) aligned with the rotation axis. Induction or creation of magnetic field is described by the induction equation:

:$\backslash frac\{\backslash partial\; \backslash mathbf\{B\}\}\{\backslash partial\; t\}\; =\; \backslash eta\; \backslash nabla^2\; \backslash mathbf\{B\}\; +\; \backslash nabla\; \backslash times\; (\backslash mathbf\{u\}\; \backslash times\; \backslash mathbf\{B\})$

where u is velocity, B is magnetic field, t is time, and $\backslash eta=1/\backslash sigma\backslash mu$ is the magnetic diffusivity with $\backslash sigma$ electrical conductivity and $\backslash mu$ permeability. The ratio of the second term on the right hand side to the first term gives the Magnetic Reynolds number, a dimensionless ratio of advection of magnetic field to diffusion.

Kinematic dynamo theory

In kinematic dynamo theory the velocity field is prescribed, instead of being a dynamic variable. This method cannot provide the time variable behavior of a fully nonlinear chaotic dynamo but is useful in studying how magnetic field strength varies with the flow structure and speed.

Using Maxwell's equations simultaneously with the curl of Ohm's Law, one can derive what is basically the linear eigenvalue equation for magnetic fields (B) which can be done when assuming that the magnetic field is independent from the velocity field. One arrives at a critical magnetic Reynolds number above which the flow strength is sufficient to amplify the imposed magnetic field, and below which it decays.

The most functional feature of kinematic dynamo theory is that it can be used to test whether a velocity field is or is not capable of dynamo action. By applying a certain velocity field to a small magnetic field, it can be determined through observation whether the magnetic field tends to grow or not in reaction to the applied flow. If the magnetic field does grow, then the system is either capable of dynamo action or is a dynamo, but if the magnetic field does not grow, then it is simply referred to as non-dynamo.

The membrane paradigm is a way of looking at black holes that allows for the material near their surfaces to be expressed in the language of dynamo theory.

Nonlinear dynamo theory

The kinematic approximation becomes invalid when the magnetic field becomes strong enough to affect the fluid motions. In that case the velocity field becomes affected by the Lorentz force, and so the induction equation is no longer linear in the magnetic field. In most cases this leads to a quenching of the amplitude of the dynamo. Such dynamos are sometimes also referred to as hydromagnetic dynamos. Virtually all dynamos in astrophysics and geophysics are hydromagnetic dynamos.

Numerical models are used to simulate fully nonlinear dynamos. A minimum of 5 equations are needed. They are as follows. The induction equation, see above. Maxwell's equation:

:$\backslash nabla\; \backslash cdot\; \backslash mathbf\{B\}=0$

The (sometimes) Boussinesq conservation of mass:

:$\backslash nabla\; \backslash cdot\; \backslash mathbf\{u\}\; =\; 0$

The (sometimes) Boussinesq conservation of momentum, also known as the Navier-Stokes equation:

:$\backslash frac\{D\backslash mathbf\{u\}\}\{Dt\}\; =\; -\backslash nabla\; p\; +\; \backslash nu\; \backslash nabla^2\; \backslash mathbf\{u\}\; +\; \backslash rho^\text{'}\backslash mathbf\{g\}\; +\; 2\backslash mathbf\{\backslash Omega\}\; \backslash times\; \backslash mathbf\{u\}\; +\; \backslash mathbf\{\backslash Omega\}\; \backslash times\; \backslash mathbf\{\backslash Omega\}\; \backslash times\; \backslash mathbf\{R\}\; +\; \backslash mathbf\{J\}\; \backslash times\; \backslash mathbf\{B\}$

where $\backslash nu$ is the kinematic viscosity, $\backslash rho^\text{'}$ is the density perturbation that provides buoyancy (for thermal convection $\backslash rho^\text{'}=\backslash alpha\backslash Delta\; T$, $\backslash Omega$ is the rotation rate of the Earth, and $\backslash mathbf\{J\}$ is the electrical current density.

Finally, a transport equation, usually of heat (sometimes of light element concentration):

:$\backslash frac\{\backslash partial\; T\}\{\backslash partial\; t\}\; =\; \backslash kappa\; \backslash nabla^2\; T\; +\backslash epsilon$

where T is temperature, $\backslash kappa=k/\backslash rho\; c\_p$ is the thermal diffusivity with k thermal conductivity, $c\_p$ heat capacity, and $\backslash rho$ density, and $\backslash epsilon$ is an optional heat source. Often the pressure is the dynamic pressure, with the hydrostatic pressure and centripetal potential removed. These equations are then non-dimensionalized, introducing the non-dimensional parameters,

:$Ra=\backslash frac\{g\backslash alpha\; T\; D^3\}\{\backslash nu\; \backslash kappa\}\; ,\; E=\backslash frac\{\backslash nu\}\{\backslash Omega\; D^2\}\; ,\; Pr=\backslash frac\{\backslash nu\}\{\backslash kappa\}\; ,\; Pm=\backslash frac\{\backslash nu\}\{\backslash eta\}$

where Ra is the Rayleigh number, E the Ekman number, Pr and Pm the Prandtl and magnetic Prandtl number. Magnetic field scaling is often in Elsasser number units $B=\backslash rho\; \backslash Omega/\backslash sigma$.

See also

Antidynamo theorem

Distributive dynamo

Dynamo

Solar dynamo

Earth's magnetic field

Maxwell's equations

Rotating magnetic field

Magnetohydrodynamics

Radiative dynamo

Shell dynamo

;Non-mainstream explanation:

Georeactor#Dynamo theory

References

Demorest, Paul. "Dynamo Theory and Earth's magnetic Field." 21 May 2001.

Fitzpatrick, Richard. "MHD Dynamo Theory." 18 May 2002.

External links

The dynamo process part of course on geomagnetism The Great Magnet, the Earth

Category:Plasma physics Category:Magnetohydrodynamics

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