Induction equation

Maxwell's equations describing the Faraday's and Ampere's laws read

${\displaystyle {\vec {\nabla }}\times {\vec {E}}=-{\partial {\vec {B}} \over \partial t},}$

and

${\displaystyle {\vec {\nabla }}\times {\vec {B}}=\mu _{0}{\vec {J}},}$

where the displacement current has been neglected as it usually has small effects in astrophysical applications as well as in most of laboratory plasmas. Here, ${\displaystyle {\vec {E}}}$, and ${\displaystyle {\vec {B}}}$ are, respectively, electric and magnetic fields, and ${\displaystyle {\vec {J}}}$ is the electric current. The electric field can be related to the current density using the Ohm's law, ${\displaystyle {\vec {E}}+{\vec {v}}\times {\vec {B}}={\vec {J}}/\sigma }$ where ${\displaystyle {\vec {v}}}$ is the velocity field, and ${\displaystyle \sigma }$ is the electric conductivity of the fluid. Combining these three equations, eliminating ${\displaystyle {\vec {E}}}$ and ${\displaystyle {\vec {J}}}$, yields the induction equation for an electrically resistive fluid:

${\displaystyle {\partial {\vec {B}} \over \partial t}=\eta \nabla ^{2}{\vec {B}}+{\vec {\nabla }}\times ({\vec {v}}\times {\vec {B}}).}$

Here, ${\displaystyle \eta =1/\mu _{0}\sigma }$ is the magnetic diffusivity (in the literature, the electrical resistivity, defined as ${\displaystyle 1/\sigma }$, is often identified with the magnetic diffusivity).

If the fluid moves with a typical speed ${\displaystyle V}$ and a typical length scale ${\displaystyle L}$, then

${\displaystyle \eta \nabla ^{2}{\vec {B}}\sim {\eta B \over L^{2}},{\vec {\nabla }}\times ({\vec {v}}\times {\vec {B}})\sim {VB \over L}.}$

The ratio of these quantities, which is a dimensionless parameter, is called the magnetic Reynolds number:

${\displaystyle R_{m}={LV \over \eta }}$.

For a fluid with infinite electric conductivity, ${\displaystyle \eta \rightarrow 0}$, the first term in the induction equation vanishes. This is equivalent to a very large magnetic Reynolds number. For example, it can be of order ${\displaystyle 10^{9}}$ in a typical star. In this case, the fluid can be called a perfect or ideal fluid. So, the induction equation for an ideal conductive fluid such as most astrophysical plasmas is

${\displaystyle {\partial {\vec {B}} \over \partial t}={\vec {\nabla }}\times ({\vec {v}}\times {\vec {B}}).}$

This is taken to be a good approximation in dynamo theory, used to explain the magnetic field evolution in the astrophysical environments such as stars, galaxies and accretion discs.

For very small magnetic Reynolds numbers, the diffusive term overcomes the convective term. For example, in an electrically resistive fluid with large values of ${\displaystyle \eta }$, the magnetic field is diffused away very fast, and the Alfvén's Theorem cannot be applied. This means magnetic energy is dissipated to heat and other types of energy. The induction equation then reads

${\displaystyle {\partial {\vec {B}} \over \partial t}=\eta \nabla ^{2}{\vec {B}}.}$

It is common to define a dissipation time scale ${\displaystyle \tau _{d}=L^{2}/\eta }$ which is the time scale for the dissipation of magnetic energy over a length scale ${\displaystyle L}$.

• Alfvén's Theorem
• Magnetohydrodynamics
• Maxwell's equations