Maxwell's equations in curved spacetime

For background material used in this article, see Covariant formulation of classical electromagnetism and Introduction to mathematics of general relativity.

Induced spacetime curvature

In physics, Maxwell's equations in curved spacetime govern the dynamics of the electromagnetic field in curved spacetime (where the metric may not be the Minkowski metric) or where one uses an arbitrary (not necessarily Cartesian) coordinate system. These equations can be viewed as a generalization of the vacuum Maxwell's equations which are normally formulated in the local coordinates of flat spacetime. But because general relativity dictates that the presence of electromagnetic fields (or energy/matter in general) induce curvature in spacetime,^[1] Maxwell's equations in flat spacetime should be viewed as a convenient approximation.

When working in the presence of bulk matter, it is preferable to distinguish between free and bound electric charges. Without that distinction, the vacuum Maxwell's equations are called the "microscopic" Maxwell's equations. When the distinction is made, they are called the macroscopic Maxwell's equations.

The electromagnetic field also admits a coordinate-independent geometric description, and Maxwell's equations expressed in terms of these geometric objects are the same in any spacetime, curved or not. Also, the same modifications are made to the equations of flat Minkowski space when using local coordinates that are not Cartesian. For example, the equations in this article can be used to write Maxwell's equations in spherical coordinates. For these reasons, it may be useful to think of Maxwell's equations in Minkowski space as a special case, rather than Maxwell's equations in curved spacetimes as a generalization.

Summary

In general relativity, the metric, g_αβ, is no longer a constant (like η_αβ as in Examples of metric tensor) but can vary in space and time, and the equations of electromagnetism in a vacuum become:

F_{\alpha \beta} \, = \, \partial_{\alpha} A_{\beta} \, - \, \partial_{\beta} A_{\alpha} \,

\mathcal{D}^{\mu\nu} \, = \, \frac{1}{\mu_{0}} \, g^{\mu\alpha} \, F_{\alpha\beta} \, g^{\beta\nu} \, \sqrt{-g} \,

J^{\mu} \, = \, \partial_\nu \mathcal{D}^{\mu \nu} \,

f_\mu \, = \, F_{\mu\nu} \, J^\nu \,

where f_μ is the density of the Lorentz force, g^αβ is the reciprocal of the metric tensor g_αβ, and g is the determinant of the metric tensor. Notice that A_α and F_αβ are (ordinary) tensors while $\mathcal{D}^{\mu\nu}$ , J^ν, and f_μ are tensor densities of weight +1. Despite the use of partial derivatives, these equations are invariant under arbitrary curvilinear coordinate transformations. Thus if one replaced the partial derivatives with covariant derivatives, the extra terms thereby introduced would cancel out. (Cf. manifest covariance#Example.)

The electromagnetic potential

The electromagnetic potential is a covariant vector, A_α which is the undefined primitive of electromagnetism. As a covariant vector, its rule for transforming from one coordinate system to another is

{\bar {A}}_{{\beta }}({\bar {x}})={\frac {\partial x^{{\gamma }}}{\partial {\bar {x}}^{{\beta }}}}A_{{\gamma }}(x)\,.

Electromagnetic field

The electromagnetic field is a covariant antisymmetric tensor of rank 2 which can be defined in terms of the electromagnetic potential by

F_{\alpha \beta} \, = \, \partial_{\alpha} A_{\beta} \, - \, \partial_{\beta} A_{\alpha} \,.

To see that this equation is invariant, we transform the coordinates (as described in the classical treatment of tensors)

\begin{align} \bar{F}_{\alpha \beta} & = \frac{\partial \bar{A}_{\beta}}{\partial \bar{x}^{\alpha}} \, - \, \frac{\partial \bar{A}_{\alpha}}{\partial \bar{x}^{\beta}} \\ & = \, \frac{\partial}{\partial \bar{x}^{\alpha}} \left( \frac{\partial x^{\gamma}}{\partial \bar{x}^{\beta}} A_{\gamma} \right) \, - \, \frac{\partial}{\partial \bar{x}^{\beta}} \left( \frac{\partial x^{\delta}}{\partial \bar{x}^{\alpha}} A_{\delta} \right) \\ & = \, \frac{\partial^2 x^{\gamma}}{\partial \bar{x}^{\alpha} \, \partial \bar{x}^{\beta}} A_{\gamma} \, + \, \frac{\partial x^{\gamma}}{\partial \bar{x}^{\beta}} \frac{\partial A_{\gamma}}{\partial \bar{x}^{\alpha}} \, - \, \frac{\partial^2 x^{\delta}}{\partial \bar{x}^{\beta} \, \partial \bar{x}^{\alpha}} A_{\delta} \, - \, \frac{\partial x^{\delta}}{\partial \bar{x}^{\alpha}} \frac{\partial A_{\delta}}{\partial \bar{x}^{\beta}} \\ & = \, \frac{\partial x^{\gamma}}{\partial \bar{x}^{\beta}} \frac{\partial x^{\delta}}{\partial \bar{x}^{\alpha}} \frac{\partial A_{\gamma}}{\partial x^{\delta}} \, - \, \frac{\partial x^{\delta}}{\partial \bar{x}^{\alpha}} \frac{\partial x^{\gamma}}{\partial \bar{x}^{\beta}} \frac{\partial A_{\delta}}{\partial x^{\gamma}} \\ & = \, \frac{\partial x^{\delta}}{\partial \bar{x}^{\alpha}} \frac{\partial x^{\gamma}}{\partial \bar{x}^{\beta}} \, \left( \frac{\partial A_{\gamma}}{\partial x^{\delta}} \, - \, \frac{\partial A_{\delta}}{\partial x^{\gamma}} \right) \\ & = \, \frac{\partial x^{\delta}}{\partial \bar{x}^{\alpha}} \frac{\partial x^{\gamma}}{\partial \bar{x}^{\beta}} \, F_{\delta \gamma} \ . \end{align}

This definition implies that the electromagnetic field satisfies

\partial_\lambda F_{\mu \nu} + \partial _\mu F_{\nu \lambda} + \partial_\nu F_{\lambda \mu} = 0 \,

which incorporates Faraday's law of induction and Gauss's law for magnetism. This is seen by

\partial_\lambda F_{\mu \nu} + \partial _\mu F_{\nu \lambda} + \partial_\nu F_{\lambda \mu} \,

= \, \partial_\lambda \partial_\mu A_\nu - \partial_\lambda \partial_\nu A_\mu + \partial_\mu \partial_\nu A_\lambda - \partial_\mu \partial_\lambda A_\nu + \partial_\nu \partial_\lambda A_\mu - \partial_\nu \partial_\mu A_\lambda \, = 0 \,.

Although there appear to be 64 equations in Faraday-Gauss, it actually reduces to just four independent equations. 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.

The Faraday-Gauss equation is sometimes written

F_{[\mu \nu ; \lambda]} \, = \, F_{[\mu \nu , \lambda]} \, = \, \frac{1}{6} \left( \partial_\lambda F_{\mu \nu} + \partial _\mu F_{\nu \lambda} + \partial_\nu F_{\lambda \mu} - \partial_\lambda F_{\nu \mu} - \partial _\mu F_{\lambda \nu} - \partial_\nu F_{\mu \lambda} \right) \,

= \, \frac{1}{3} \left( \partial_\lambda F_{\mu \nu} + \partial _\mu F_{\nu \lambda} + \partial_\nu F_{\lambda \mu} \right) = 0 \,

where the semicolon indicates a covariant derivative, comma indicate a partial derivative, and square brackets indicate anti-symmetrization (see Ricci calculus for the notation). The covariant derivative of the electromagnetic field is

F_{\alpha \beta ; \gamma} \, = \, F_{\alpha \beta , \gamma} - {\Gamma^{\mu}}_{\alpha \gamma} F_{\mu \beta} - {\Gamma^{\mu}}_{\beta \gamma} F_{\alpha \mu} \,

where Γ^α_{β γ} is the Christoffel symbol which is symmetric in its lower indices.

Electromagnetic displacement

The electric displacement field, D and the auxiliary magnetic field, H form an antisymmetric contravariant rank 2 tensor density of weight +1. In a vacuum, this is given by

\mathcal{D}^{\mu \nu} \, = \, \frac{1}{\mu_{0}} \, g^{\mu \alpha} \, F_{\alpha \beta} \, g^{\beta \nu} \, \sqrt{-g} \,.

This equation is the only place where the metric (and thus gravity) enters into the theory of electromagnetism. Furthermore, the equation is invariant under a change of scale, that is, multiplying the metric by a constant has no effect on this equation. Consequently, gravity can only affect electromagnetism by changing the speed of light relative to the global coordinate system being used. Light is only deflected by gravity because it is slower when near to massive bodies. So it is as if gravity increased the index of refraction of space near massive bodies.

More generally, in materials where the magnetization–polarization tensor is non-zero, we have

\mathcal{D}^{\mu \nu} \, = \, \frac{1}{\mu_{0}} \, g^{\mu \alpha} \, F_{\alpha \beta} \, g^{\beta \nu} \, \sqrt{-g} \, - \, \mathcal{M}^{\mu \nu} \,.

The transformation law for electromagnetic displacement is

\bar{\mathcal{D}}^{\mu \nu} \, = \, \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, \frac{\partial \bar{x}^{\nu}}{\partial x^{\beta}} \, \mathcal{D}^{\alpha \beta} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \,

where the Jacobian determinant is used. If the magnetization-polarization tensor is used, it has the same transformation law as the electromagnetic displacement.

Electric current

The electric current is the divergence of the electromagnetic displacement. In a vacuum,

J^{\mu} \, = \, \partial_{\nu} \mathcal{D}^{\mu \nu} \,.

If magnetization-polarization is used, then this just gives the free portion of the current

J^{\mu}_{\text{free}} \, = \, \partial_{\nu} \mathcal{D}^{\mu \nu} \,.

This incorporates Ampere's Law and Gauss's Law.

In either case, the fact that the electromagnetic displacement is antisymmetric implies that the electric current is automatically conserved

\partial_{\mu} J^{\mu} \, = \, \partial_{\mu} \partial_{\nu} \mathcal{D}^{\mu \nu} = 0 \,

because the partial derivatives commute.

The Ampere-Gauss definition of the electric current is not sufficient to determine its value because the electromagnetic potential (from which it was ultimately derived) has not been given a value. Instead, the usual procedure is to equate the electric current to some expression in terms of other fields, mainly the electron and proton, and then solve for the electromagnetic displacement, electromagnetic field, and electromagnetic potential.

The electric current is a contravariant vector density, and as such it transforms as follows

\bar{J}^{\mu} \, = \, \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, J^{\alpha} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \,.

Verification of this transformation law

\begin{align} \bar{J}^{\mu} \, & = \, \frac{\partial}{\partial \bar{x}^{\nu}} \left( \bar{\mathcal{D}}^{\mu \nu} \right) \, = \, \frac{\partial}{\partial \bar{x}^{\nu}} \left( \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, \frac{\partial \bar{x}^{\nu}}{\partial x^{\beta}} \, \mathcal{D}^{\alpha \beta} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \right) \\ & = \, \frac{\partial^2 \bar{x}^{\mu}}{\partial \bar{x}^{\nu} \partial x^{\alpha}} \, \frac{\partial \bar{x}^{\nu}}{\partial x^{\beta}} \, \mathcal{D}^{\alpha \beta} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \, + \, \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, \frac{\partial^2 \bar{x}^{\nu}}{\partial \bar{x}^{\nu} \partial x^{\beta}} \, \mathcal{D}^{\alpha \beta} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \\ & + \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, \frac{\partial \bar{x}^{\nu}}{\partial x^{\beta}} \, \frac{\partial \mathcal{D}^{\alpha \beta}}{\partial \bar{x}^{\nu}} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \, + \, \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, \frac{\partial \bar{x}^{\nu}}{\partial x^{\beta}} \, \mathcal{D}^{\alpha \beta} \, \frac{\partial}{\partial \bar{x}^{\nu}} \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \\ & = \, \frac{\partial^2 \bar{x}^{\mu}}{\partial x^{\beta} \partial x^{\alpha}} \, \mathcal{D}^{\alpha \beta} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \, + \, \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, \frac{\partial^2 \bar{x}^{\nu}}{\partial \bar{x}^{\nu} \partial x^{\beta}} \, \mathcal{D}^{\alpha \beta} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \\ & + \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, \frac{\partial \mathcal{D}^{\alpha \beta}}{\partial x^{\beta}} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \, + \, \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, \frac{\partial \bar{x}^{\nu}}{\partial x^{\beta}} \, \mathcal{D}^{\alpha \beta} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \frac{\partial \bar{x}^{\rho}}{\partial x^{\sigma}} \frac{\partial^2 x^{\sigma}}{\partial \bar{x}^{\nu} \partial \bar{x}^{\rho}}\\ & = \, 0 \, + \, \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, \frac{\partial^2 \bar{x}^{\nu}}{\partial \bar{x}^{\nu} \partial x^{\beta}} \, \mathcal{D}^{\alpha \beta} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \\ & + \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, J^{\alpha} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \, + \, \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, \mathcal{D}^{\alpha \beta} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \frac{\partial \bar{x}^{\rho}}{\partial x^{\sigma}} \frac{\partial^2 x^{\sigma}}{\partial x^{\beta} \partial \bar{x}^{\rho}} \\ & = \, \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, J^{\alpha} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \, + \, \frac{\partial \bar{x}^{\mu}}{\partial x^{\alpha}} \, \mathcal{D}^{\alpha \beta} \, \det \left[ \frac{\partial x^{\sigma}}{\partial \bar{x}^{\rho}} \right] \left( \frac{\partial^2 \bar{x}^{\nu}} {\partial \bar{x}^{\nu} \partial x^{\beta}} \, + \, \frac{\partial \bar{x}^{\rho}}{\partial x^{\sigma}} \frac{\partial^2 x^{\sigma}}{\partial x^{\beta} \partial \bar{x}^{\rho}} \right) \end{align}

So all that remains is to show that

\frac{\partial^2 \bar{x}^{\nu}}{\partial \bar{x}^{\nu} \partial x^{\beta}} \, + \, \frac{\partial \bar{x}^{\rho}}{\partial x^{\sigma}} \frac{\partial^2 x^{\sigma}}{\partial x^{\beta} \partial \bar{x}^{\rho}} \, = \, 0 \,

which is a version of a known theorem (see Inverse functions and differentiation#Higher derivatives).

\begin{align} \frac{\partial^2 \bar{x}^{\nu}}{\partial \bar{x}^{\nu} \partial x^{\beta}} \, + \, \frac{\partial \bar{x}^{\rho}}{\partial x^{\sigma}} \frac{\partial^2 x^{\sigma}}{\partial x^{\beta} \partial \bar{x}^{\rho}} & = \, \frac{\partial x^{\sigma}}{\partial \bar{x}^{\nu}} \frac{\partial^2 \bar{x}^{\nu}}{\partial x^{\sigma} \partial x^{\beta}} \, + \, \frac{\partial \bar{x}^{\nu}}{\partial x^{\sigma}} \frac{\partial^2 x^{\sigma}}{\partial x^{\beta} \partial \bar{x}^{\nu}} \\ & = \, \frac{\partial x^{\sigma}}{\partial \bar{x}^{\nu}} \frac{\partial^2 \bar{x}^{\nu}}{\partial x^{\beta} \partial x^{\sigma}} \, + \, \frac{\partial^2 x^{\sigma}}{\partial x^{\beta} \partial \bar{x}^{\nu}} \frac{\partial \bar{x}^{\nu}}{\partial x^{\sigma}} \, = \, \frac{\partial}{\partial x^{\beta}} \left( \frac{\partial x^{\sigma}}{\partial \bar{x}^{\nu}} \, \frac{\partial \bar{x}^{\nu}}{\partial x^{\sigma}} \right) \\ & = \, \frac{\partial}{\partial x^{\beta}} \left( \, \frac{\partial \bar{x}^{\nu}}{\partial \bar{x}^{\nu}} \right) \, = \, \frac{\partial}{\partial x^{\beta}} \left( \mathbf{4} \right) \, = \, 0 \,. \end{align}

Lorentz force density

The density of the Lorentz force is a covariant vector density given by

f_{\mu} \, = \, F_{\mu \nu} \, J^{\nu} \,.

The force on a test particle subject only to gravity and electromagnetism is

\frac{d p_{\alpha}}{d t} \, = \, \Gamma^{\beta}_{\alpha \gamma} \, p_{\beta} \, \frac{d x^{\gamma}}{d t} \, + \, q \, F_{\alpha \gamma} \, \frac{d x^{\gamma}}{d t} \,

where p_α is the linear 4-momentum of the particle, t is any time coordinate parameterizing the world line of the particle, Γ^β_αγ is the Christoffel symbol (gravitational force field), and q is the electric charge of the particle.

This equation is invariant under a change in the time coordinate; just multiply by $d t/d \bar{t}$ and use the chain rule. It is also invariant under a change in the x coordinate system.

Using the transformation law for the Christoffel symbol

\bar{\Gamma}^{\beta}_{\alpha \gamma} \, = \, \frac{\partial \bar{x}^{\beta}}{\partial x^{\epsilon}} \, \frac{\partial x^{\delta}}{\partial \bar{x}^{\alpha}} \, \frac{\partial x^{\zeta}}{\partial \bar{x}^{\gamma}} \, \Gamma^{\epsilon}_{\delta \zeta} \, + \frac{\partial \bar{x}^{\beta}}{\partial x^{\eta}}\, \frac{\partial^2 x^{\eta}}{\partial \bar{x}^{\alpha} \partial \bar{x}^{\gamma}} \,

we get

\begin{align} & \frac{d \bar{p}_{\alpha}}{d t} \, - \, \bar{\Gamma}^{\beta}_{\alpha \gamma} \, \bar{p}_{\beta} \, \frac{d \bar{x}^{\gamma}}{d t} \, - \, q \, \bar{F}_{\alpha \gamma} \, \frac{d \bar{x}^{\gamma}}{d t} \\ & = \, \frac{d}{d t} \left( \frac{\partial x^{\delta}}{\partial \bar{x}^{\alpha}} \, p_{\delta} \right) \, - \, \left( \frac{\partial \bar{x}^{\beta}}{\partial x^{\theta}} \, \frac{\partial x^{\delta}}{\partial \bar{x}^{\alpha}} \, \frac{\partial x^{\iota}}{\partial \bar{x}^{\gamma}} \, \Gamma^{\theta}_{\delta \iota} + \, \frac{\partial \bar{x}^{\beta}}{\partial x^{\eta}}\, \frac{\partial^2 x^{\eta}}{\partial \bar{x}^{\alpha} \partial \bar{x}^{\gamma}} \right) \, \frac{\partial x^{\epsilon}}{\partial \bar{x}^{\beta}} \, p_{\epsilon} \, \frac{\partial \bar{x}^{\gamma}}{\partial x^{\zeta}} \, \frac{d x^{\zeta}}{d t} \, - \, q \, \frac{\partial x^{\delta}}{\partial \bar{x}^{\alpha}} \, F_{\delta \zeta} \, \frac{d x^{\zeta}}{d t} \\ & = \, \frac{\partial x^{\delta}}{\partial \bar{x}^{\alpha}} \, \left( \frac{d p_{\delta}}{d t} \, - \, \Gamma^{\epsilon}_{\delta \zeta} \, p_{\epsilon} \, \frac{d x^{\zeta}}{d t} \, - \, q \, F_{\delta \zeta} \, \frac{d x^{\zeta}}{d t} \right) + \frac{d}{d t} \left( \frac{\partial x^{\delta}}{\partial \bar{x}^{\alpha}} \right) \, p_{\delta} \, - \, \left( \frac{\partial \bar{x}^{\beta}}{\partial x^{\eta}}\, \frac{\partial^2 x^{\eta}}{\partial \bar{x}^{\alpha} \partial \bar{x}^{\gamma}} \right) \, \frac{\partial x^{\epsilon}}{\partial \bar{x}^{\beta}} \, p_{\epsilon} \, \frac{\partial \bar{x}^{\gamma}}{\partial x^{\zeta}} \, \frac{d x^{\zeta}}{d t} \\ & = \, 0 \, + \, \frac{d}{d t} \left( \frac{\partial x^{\delta}}{\partial \bar{x}^{\alpha}} \right) \, p_{\delta} \, - \, \frac{\partial^2 x^{\epsilon}}{\partial \bar{x}^{\alpha} \partial \bar{x}^{\gamma}} p_{\epsilon} \, \frac{d \bar{x}^{\gamma}}{d t} \, = \, 0 \ . \end{align}

Lagrangian

In a vacuum, the Lagrangian for classical electrodynamics (in joules/meter³) is a scalar density

\mathcal{L} \, = \, - \frac{1}{4 \mu_0} \, F_{\alpha \beta} \, F^{\alpha \beta} \, \sqrt{- g} \, + \, A_{\alpha} \, J^{\alpha} \,

where

F^{\alpha \beta} = g^{\alpha \gamma} F_{\gamma \delta} g^{\delta \beta} \,.

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.

If we separate free currents from bound currents, the Lagrangian becomes

\mathcal{L} \, = \, - \frac{1}{4 \mu_0} \, F_{\alpha \beta} \, F^{\alpha \beta} \, \sqrt{- g} \, + \,A_{\alpha} \, J^{\alpha}_{\text{free}} \, + \, \frac12 \, F_{\alpha \beta} \, \mathcal{M}^{\alpha \beta} \,.

Electromagnetic stress–energy tensor

Main article: Electromagnetic stress–energy tensor

As part of the source term in the Einstein field equations, the electromagnetic stress–energy tensor is a covariant symmetric tensor

T_{\mu \nu} \, = \, - \frac{1}{\mu_0} ( F_{\mu \alpha} g^{\alpha \beta} F_{\beta \nu} \, - \, \frac{1}{4} g_{\mu \nu} \, F_{\sigma \alpha} g^{\alpha \beta} F_{\beta \rho} g^{\rho \sigma} ) \,

using a metric of signature (-,+,+,+). If using the metric with signature (+,-,-,-), the expression for $T_{\mu \nu }$ will have opposite sign. The stress–energy tensor is trace-free

T_{\mu \nu} g^{\mu \nu} \, = \, 0 \,

because electromagnetism propagates at the invariant speed.

In the expression for the conservation of energy and linear momentum, the electromagnetic stress–energy tensor is best represented as a mixed tensor density

\mathfrak{T}_{\mu}^{\nu} = T_{\mu \gamma} \, g^{\gamma \nu} \, \sqrt{-g}.

From the equations above, one can show that

{\mathfrak{T}_{\mu}^{\nu}}_{; \nu} \, + \, f_{\mu} \, = \, 0 \,

where the semicolon indicates a covariant derivative.

This can be rewritten as

- {\mathfrak{T}_{\mu}^{\nu}}_{, \nu} \, = \, - \Gamma^{\sigma}_{\mu \nu} \mathfrak{T}_{\sigma}^{\nu} \, + \, f_{\mu} \,

which says that the decrease in the electromagnetic energy is the same as the work done by the electromagnetic field on the gravitational field plus the work done on matter (via the Lorentz force), and similarly the rate of decrease in the electromagnetic linear momentum is the electromagnetic force exerted on the gravitational field plus the Lorentz force exerted on matter.

Derivation of conservation law

\begin{align} {\mathfrak{T}_{\mu}^{\nu}}_{; \nu} \, + \, f_{\mu} \, & = \, - \frac{1}{\mu_0} ( F_{\mu \alpha ; \nu} g^{\alpha \beta} F_{\beta \gamma} g^{\gamma \nu} \, + \, F_{\mu \alpha} g^{\alpha \beta} F_{\beta \gamma ; \nu} g^{\gamma \nu} \, - \, \frac12 \delta_{\mu}^{\nu} \, F_{\sigma \alpha ; \nu} g^{\alpha \beta} F_{\beta \rho} g^{\rho \sigma} ) \sqrt{- g} \\ & + \frac{1}{\mu_{0}} \, F_{\mu \alpha} \, g^{\alpha \beta} \, F_{\beta \gamma ; \nu} \, g^{\gamma \nu} \, \sqrt{-g} \\ & = \, - \frac{1}{\mu_0} ( F_{\mu \alpha ; \nu} F^{\alpha \nu} \, - \, \frac12 F_{\sigma \alpha ; \mu} F^{\alpha \sigma} ) \sqrt{- g}\\ & = \, - \frac{1}{\mu_0} ( (- F_{\nu \mu ; \alpha} - F_{\alpha \nu ; \mu}) F^{\alpha \nu} \, - \, \frac12 F_{\sigma \alpha ; \mu} F^{\alpha \sigma} ) \sqrt{- g} \\ & = \, - \frac{1}{\mu_0} ( F_{\mu \nu ; \alpha} F^{\alpha \nu} - F_{\alpha \nu ; \mu} F^{\alpha \nu} \, + \, \frac12 F_{\sigma \alpha ; \mu} F^{\sigma \alpha} ) \sqrt{- g} \\ & = \, - \frac{1}{\mu_0} ( F_{\mu \alpha ; \nu} F^{\nu \alpha} - \frac12 F_{\alpha \nu ; \mu} F^{\alpha \nu} ) \sqrt{- g} \\ & = \, - \frac{1}{\mu_0} (- F_{\mu \alpha ; \nu} F^{\alpha \nu} \, + \, \frac12 F_{\sigma \alpha ; \mu} F^{\alpha \sigma} ) \sqrt{- g} \ , \end{align}

which is zero because it is the negative of itself (see four lines above).

Electromagnetic wave equation

The nonhomogeneous electromagnetic wave equation in terms of the field tensor is modified from the special relativity form to

\Box F_{ab} \ \stackrel{\mathrm{def}}{=}\ F_{ab;}{}^d{}_d = \, -2 R_{acbd} F^{cd} + R_{ae}F^e{}_b - R_{be}F^e{}_a + J_{a;b} - J_{b;a}

where R_acbd is the covariant form of the Riemann tensor and $\Box$ is a generalization of the d'Alembertian operator for covariant derivatives. Using

\Box A^{a} = {{A^{a; }}^{b}}_{ b}

Maxwell's source equations can be written in terms of the 4-potential [ref 2, p. 569] as,

\Box A^{a} - {A^{b;a}}_{ b} = - \mu_0 J^{ a }

or, assuming the generalization of the Lorenz gauge in curved spacetime

{A^{ a }}_{ ; a } = 0 \ ,

\Box A^{a} = - \mu_0 J^{ a } + {R^{ a }}_{ b } A^{ b }

where $R_{ a b } \ \stackrel{\mathrm{def}}{=}\ {R^{ s }}_{ a s b }$ is the Ricci curvature tensor.

This the same form of the wave equation as in flat spacetime, except that the derivatives are replaced by covariant derivatives and there is an additional term proportional to the curvature. The wave equation in this form also bears some resemblance to the Lorentz force in curved spacetime where A^a plays the role of the 4-position.

Nonlinearity of Maxwell's equations in a dynamic spacetime

When Maxwell's equations are treated in a background independent manner, that is, when the spacetime metric is taken to be a dynamical variable dependent on the electromagnetic field, then the electromagnetic wave equation and Maxwell's equations are nonlinear. This can be seen by noting that the curvature tensor depends on the stress–energy tensor through the Einstein field equation

G_{ab} = \frac{8 \pi G} {c^4} T_{ab}

where

{G}_{a b} \ \stackrel{\mathrm{def}}{=}\ {R}_{a b} - {1 \over 2} {R} g_{a b}

is the Einstein tensor, G is the gravitational constant, g_ab is the metric tensor, and R (scalar curvature) is the trace of the Ricci curvature tensor. The stress–energy tensor is composed of the stress-energy from particles, but also stress-energy from the electromagnetic field. This generates the nonlinearity.

Geometric formulation

In the differential geometric formulation of the electromagnetic field, the antisymmetric Faraday tensor can be considered as the Faraday 2-form F. In this view, one of Maxwell's two equations is dF= 0, where d is the exterior derivative operator. This equation is completely coordinate and metric independent and says that the electro-magnetic flux through a closed two dimensional surface in space time is topological, more precisely, depends only on its homology class (a generalization of the integral form of Gauss law and Maxwell-Faraday equation as the homology class in Minkowski space is automatically 0). By the Poincaré lemma, this equation implies, (at least locally) that there exists a 1-form A satisfying F = d A. The other Maxwell equation is d * F = J. In this context, J is the current 3-form (or even more precise, twisted three form), the asterisk * denotes the Hodge star operator, and d is the exterior derivative operator. The dependence of Maxwell's equation on the metric of spacetime lies in the Hodge star operator * on two forms, which is conformally invariant. Written this way, Maxwell's equation is the same in any space time, manifestly coordinate invariant, and convenient to use (even in Minkowski space or Euclidean space and time especially with curvilinear coordinates).

An even more geometric interpretation is that the Faraday two form F is (up to a factor i) the curvature 2-form $F(\nabla)$ of a U(1)-connection $\nabla$ on a principal U(1)-bundle whose sections represent charged fields. The connection is much like the vector potential since every connection can be written as $\nabla = \nabla_0 + iA$ for a "base" connection $\nabla_0$ and F = F₀ + d A. In this view, the Maxwell "equation", d F= 0, is a mathematical identity known as the Bianchi identity. The equation d * F = J is the only equation with any physical content in this formulation. This point of view is particularly natural when considering charged fields or quantum mechanics. It can be interpreted as saying that, much like gravity can be understood as being the result of the necessity of a connection to parallel transport vectors at different points, electromagnetic phenomena, or more subtle quantum effects like the Aharanov-Bohm effect, can be understood as a result from the necessity of a connection to parallel transport charged fields or wave sections at different points. In fact, just as the Riemann tensor is the holonomy of the Levi Civita connection along an infinitesimal closed curve, the curvature of the connection is the holonomy of the U(1)-connection.

Notes

↑ http://www.springerlink.com/content/h224886u7651v774/

References

Einstein, A. (1961). Relativity: The Special and General Theory. New York: Crown. ISBN 0-517-02961-8.
Misner, Charles W.; 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 ed.). Oxford: Pergamon. ISBN 0-08-018176-7.
Feynman, R. P.; Moringo, F. B.; Wagner, W. G. (1995). Feynman Lectures on Gravitation. Addison-Wesley. ISBN 0-201-62734-5.

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Glossary of tensor theory

Scope

Mathematics	coordinate system multilinear algebra Euclidean geometry tensor algebra differential geometry exterior calculus tensor calculus

Physics Engineering	continuum mechanics electromagnetism transport phenomena general relativity computer vision

Notation

Tensor definitions

Operations

Related abstractions

Notable tensors

Mathematics	Kronecker delta Levi-Civita symbol metric tensor nonmetricity tensor Christoffel symbols Ricci curvature Riemann curvature tensor Weyl tensor torsion tensor

Physics	moment of inertia angular momentum tensor spin tensor Cauchy stress tensor stress–energy tensor EM tensor gluon field strength tensor Einstein tensor metric tensor (GR)

Mathematicians

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