# Covariant formulation of classical electromagnetism

The **covariant formulation of classical electromagnetism** refers to ways of writing the laws of classical electromagnetism (in particular, Maxwell's equations and the Lorentz force) in a form that is manifestly invariant under Lorentz transformations, in the formalism of special relativity using rectilinear inertial coordinate systems. These expressions both make it simple to prove that the laws of classical electromagnetism take the same form in any inertial coordinate system, and also provide a way to translate the fields and forces from one frame to another. However, this is not as general as Maxwell's equations in curved spacetime or non-rectilinear coordinate systems.

This article uses the classical treatment of tensors and Einstein summation convention throughout and the Minkowski metric has the form diag (+1, −1, −1, −1). Where the equations are specified as holding in a vacuum, one could instead regard them as the formulation of Maxwell's equations in terms of *total* charge and current.

For a more general overview of the relationships between classical electromagnetism and special relativity, including various conceptual implications of this picture, see Classical electromagnetism and special relativity.

## Covariant objects

### Preliminary 4-vectors

Lorentz tensors of the following kinds may be used in this article to describe bodies or particles:

- where
*γ*(**u**) is the Lorentz factor at the 3-velocity**u**.

- where is 3-momentum, is the total energy, and is rest mass.

- The d'Alembertian operator is denoted .

The signs in the following tensor analysis depend on the convention used for the metric tensor. The convention used here is `+−−−`, corresponding to the Minkowski metric tensor:

### Electromagnetic tensor

The electromagnetic tensor is the combination of the electric and magnetic fields into a covariant antisymmetric tensor whose entries are B-field quantities.
^{[1]}

and the result of raising its indices is

where **E** is the electric field, **B** the magnetic field, and *c* the speed of light.

### Four-current

The four-current is the contravariant four-vector which combines electric charge density *ρ* and electric current density **j**:

### Four-potential

The electromagnetic four-potential is a covariant four-vector containing the electric potential (also called the scalar potential) *ϕ* and magnetic vector potential (or vector potential) **A**, as follows:

The differential of the electromagnetic potential is

### Electromagnetic stress–energy tensor

The electromagnetic stress–energy tensor can be interpreted as the flux density of the momentum 4-vector, and is a contravariant symmetric tensor that is the contribution of the electromagnetic fields to the overall stress–energy tensor:

where *ε*_{0} is the electric permittivity of vacuum, *μ*_{0} is the magnetic permeability of vacuum, the Poynting vector is

and the Maxwell stress tensor is given by

The electromagnetic field tensor *F* constructs the electromagnetic stress–energy tensor *T* by the equation:

where *η* is the Minkowski metric tensor. Notice that we use the fact that

which is predicted by Maxwell's equations.

## Maxwell's equations *in vacuo*

In vacuo (or for the microscopic equations, not including macroscopic material descriptions), Maxwell's equations can be written as two tensor equations.

The two inhomogeneous Maxwell's equations, Gauss's Law and Ampère's law (with Maxwell's correction) combine into (with +−−− metric):^{[2]}

while the homogeneous equations – Faraday's law of induction and Gauss's law for magnetism combine to form:

where *F*^{αβ} is the electromagnetic tensor, *J*^{α} is the 4-current, *ε*^{αβγδ} is the Levi-Civita symbol, and the indices behave according to the Einstein summation convention.

The first tensor equation corresponds to four scalar equations, one for each value of *β*. The second tensor equation actually corresponds to 4^{3} = 64 different scalar equations, but only four of these are independent. Using the antisymmetry of the electromagnetic field one can either reduce to an identity (0 = 0) or render redundant all the equations except for those with *λ*, *μ*, *ν* = either 1,2,3 or 2,3,0 or 3,0,1 or 0,1,2.

Using the antisymmetric tensor notation and comma notation for the partial derivative (see Ricci calculus), the second equation can also be written more compactly as:

In the absence of sources, Maxwell's equations reduce to:

which is an electromagnetic wave equation in the field strength tensor.

### Maxwell's equations in the Lorenz gauge

The Lorenz gauge condition is a Lorentz-invariant gauge condition. (This can be contrasted with other gauge conditions such as the Coulomb gauge, which if it holds in one inertial frame it will generally not hold in any other.) It is expressed in terms of the four-potential as follows:

In the Lorenz gauge, the microscopic Maxwell's equations can be written as:

## Lorentz force

### Charged particle

Electromagnetic (EM) fields affect the motion of electrically charged matter: due to the Lorentz force. In this way, EM fields can be detected (with applications in particle physics, and natural occurrences such as in aurorae). In relativistic form, the Lorentz force uses the field strength tensor as follows.^{[3]}

Expressed in terms of coordinate time *t*, it is:

where *p*_{α} is the four-momentum, *q* is the charge, and *x*^{β} is the position.

In the co-moving reference frame, this yields the 4-force

where *u*^{β} is the four-velocity, and τ is the particle's proper time, which is related to coordinate time by *dt* = γ*d*τ.

### Charge continuum

The density of force due to electromagnetism, whose spatial part is the Lorentz force, is given by

and is related to the electromagnetic stress–energy tensor by

## Conservation laws

### Electric charge

The continuity equation:

expresses charge conservation.

### Electromagnetic energy–momentum

Using the Maxwell equations, one can see that the electromagnetic stress–energy tensor (defined above) satisfies the following differential equation, relating it to the electromagnetic tensor and the current four-vector

or

which expresses the conservation of linear momentum and energy by electromagnetic interactions.

## Covariant objects in matter

### Free and bound 4-currents

In order to solve the equations of electromagnetism given here, it is necessary to add information about how to calculate the electric current, *J*^{ν} Frequently, it is convenient to separate the current into two parts, the free current and the bound current, which are modeled by different equations;

where

Maxwell's macroscopic equations have been used, in addition the definitions of the electric displacement **D** and the magnetic intensity **H**:

where **M** is the magnetization and **P** the electric polarization.

### Magnetization-polarization tensor

The bound current is derived from the **P** and **M** fields which form an antisymmetric contravariant magnetization-polarization tensor ^{[1]}

which determines the bound current

### Electric displacement tensor

If this is combined with *F*^{μν} we get the antisymmetric contravariant electromagnetic displacement tensor which combines the **D** and **H** fields as follows:

The three field tensors are related by:

which is equivalent to the definitions of the **D** and **H** fields given above.

## Maxwell's equations in matter

The result is that Ampère's law,

- ,

and Gauss's law,

- ,

combine into one equation:

The bound current and free current as defined above are automatically and separately conserved

### Constitutive equations

#### Vacuum

In vacuum, the constitutive relations between the field tensor and displacement tensor are:

Antisymmetry reduces these 16 equations to just six independent equations. Because it is usual to define *F*^{μν} by

the constitutive equations may, in *vacuum*, be combined with the Gauss–Ampère law to get:

The electromagnetic stress–energy tensor in terms of the displacement is:

where *δ _{α}^{π}* is the Kronecker delta. When the upper index is lowered with

*η*, it becomes symmetric and is part of the source of the gravitational field.

#### Linear, nondispersive matter

Thus we have reduced the problem of modeling the current, *J*^{ν} to two (hopefully) easier problems — modeling the free current, *J*^{ν}_{free} and modeling the magnetization and polarization,
. For example, in the simplest materials at low frequencies, one has

where one is in the instantaneously comoving inertial frame of the material, σ is its electrical conductivity, χ_{e} is its electric susceptibility, and χ_{m} is its magnetic susceptibility.

The constitutive relations between the
and *F* tensors, proposed by Minkowski for a linear materials (that is, **E** is proportional to **D** and **B** proportional to **H**), are:^{[4]}

where *u* is the 4-velocity of material, ε and μ are respectively the proper permittivity and permeability of the material (i.e. in rest frame of material),
and denotes the Hodge dual.

## Lagrangian for classical electrodynamics

### Vacuum

The Lagrangian density for classical electrodynamics is

In the interaction term, the four-current should be understood as an abbreviation of many terms expressing the electric currents of other charged fields in terms of their variables; the four-current is not itself a fundamental field.

The Euler–Lagrange equation for the electromagnetic Lagrangian density can be stated as follows:

Noting

- ,

the expression inside the square bracket is

The second term is

Therefore, the electromagnetic field's equations of motion are

which is one of the Maxwell equations above.

### Matter

Separating the free currents from the bound currents, another way to write the Lagrangian density is as follows:

Using Euler–Lagrange equation, the equations of motion for can be derived.

The equivalent expression in non-relativistic vector notation is

## See also

- Covariant classical field theory
- Electromagnetic tensor
- Electromagnetic wave equation
- Liénard–Wiechert potential for a charge in arbitrary motion
- Moving magnet and conductor problem
- Nonhomogeneous electromagnetic wave equation
- Proca action
- Quantum electrodynamics
- Relativistic electromagnetism
- Stueckelberg action
- Wheeler–Feynman absorber theory

## Notes and references

- 1 2 Vanderlinde, Jack (2004),
*classical electromagnetic theory*, Springer, pp. 313–328, ISBN 9781402026997 - ↑ Classical Electrodynamics by Jackson, 3rd Edition, Chapter 11 Special Theory of Relativity
- ↑ The assumption is made that no forces other than those originating in
**E**and**B**are present, that is, no gravitational, weak or strong forces. - ↑ D.J. Griffiths (2007).
*Introduction to Electrodynamics*(3rd ed.). Dorling Kindersley. p. 563. ISBN 81-7758-293-3.

## Further reading

- Einstein, A. (1961).
*Relativity: The Special and General Theory*. New York: Crown. ISBN 0-517-02961-8. - Misner, Charles; Thorne, Kip S.; Wheeler, John Archibald (1973).
*Gravitation*. San Francisco: W. H. Freeman. ISBN 0-7167-0344-0. - Landau, L. D.; Lifshitz, E. M. (1975).
*Classical Theory of Fields (Fourth Revised English Edition)*. Oxford: Pergamon. ISBN 0-08-018176-7. - R. P. Feynman; F. B. Moringo; W. G. Wagner (1995).
*Feynman Lectures on Gravitation*. Addison-Wesley. ISBN 0-201-62734-5.