Metric tensor (general relativity)

This article discusses metrics in general relativity, for a discussion of metrics in general, see metric tensor.

In general relativity, the metric tensor (or simply the metric) is the fundamental object of study. It may loosely be thought of as a generalization of the gravitational field familiar from Newtonian gravitation. The metric captures all the geometric and causal structure of spacetime. Using the metric one can define such notions as distance, volume, angle, future, past, and curvature.

Notation and conventions: Throughout this article we work with a metric signature that is mostly positive (-+++); see sign convention. As is customary is relativity, we work in units where the speed of light c = 1. The gravitation constant G will be kept explicit. We also make use of the summation convention, where repeated indicies are automatically summed over.

Definition

Mathematically, spacetime is represented by a 4-dimensional differentiable manifold M and the metric is given as a covariant, second-rank, symmetric tensor on M, conventionally denoted by g. Moreover the metric is required to be nondegenerate with signature (-+++). A manifold M equipped with such a metric is called a Lorentzian manifold.

Explicitly, the metric is a symmetric bilinear form on each tangent space of M which varies in a smooth (or differentiable) manner from point to point. Given two tangent vectors u and v and a point x in M, the metric can be evaluted on u and v to give a real number:

${\displaystyle g_{x}(u,v)=g_{x}(v,u)\in \mathbb {R} .}$ 

This can be thought of as a generalization of the dot product in ordinary Euclidean space. This analogy is not exact, however. Rather, than Euclidean space — where the dot product is positive definite — the metric gives each tangent space the structure of Minkowski space.

Local coordinates and matrix representations

Physicists usually work in local coordinates (i.e. coordinates defined on some local patch of M). In local coordinates ${\displaystyle x^{\mu }}$  (where ${\displaystyle \mu }$  is an index which runs from 0 to 3) the metric can be written in the form

${\displaystyle \mathbf {g} =g_{\mu \nu }{\tilde {d}}x^{\mu }\otimes {\tilde {d}}x^{\nu }.}$ 

The factors ${\displaystyle {\tilde {d}}x^{\mu }}$  are one-form gradients of the scalar coordinate fields ${\displaystyle x^{\mu }}$ . The metric is thus a linear combination of tensor products of one-form gradients of coordinates. The coefficients ${\displaystyle g_{\mu \nu }}$  are a set of 16 real-valued functions (since the tensor g is actually a tensor field defined at all points of a spacetime manifold). In order for the metric to be symmetric we must have

${\displaystyle g_{\mu \nu }=g_{\nu \mu }\,}$ 

giving 10 independent coefficients.

If the local coordinates are specified, or understood from context, the metric can be written as a 4×4 symmetric matrix with entries ${\displaystyle g_{\mu \nu }}$ . The nondegeneracy of ${\displaystyle g_{\mu \nu }}$  means that this matrix is non-singular (i.e. has non-vanishing determinant), while the Lorentzian signature of g implies that the matrix has one negative and three positive eigenvalues. Note that physicists often refer to this matrix or the coordinates ${\displaystyle g_{\mu \nu }}$  themselves as the metric (see, however, abstract index notation).

With the the quantity ${\displaystyle dx^{\mu }}$  being an infinitesimal coordinate displacement, the metric acts as an infinitesimal invariant interval squared or line element. For this reason one often sees the notation ${\displaystyle ds^{2}}$  for the metric:

${\displaystyle ds^{2}=g_{\mu \nu }dx^{\mu }dx^{\nu }.\,}$ 

In general relativity, the terms metric and line element are often used interchangeably.

${\displaystyle ds^{2}}$  imparts information about the causal structure of the spacetime. When ${\displaystyle ds^{2}<0}$ , the interval is timelike and the square root of the absolute value of ds² is an incremental proper time. Only timelike intervals can be physically traveled by a massive object. When ${\displaystyle ds^{2}=0}$ , the interval is lightlike, and can only be traveled by light. When ${\displaystyle ds^{2}>0}$ , the interval is spacelike and the square root of ds² acts as an incremental proper length. Spacelike intervals cannot be traveled, since they connect events that are out of each other's light cones. Events can be causally related only if they are within each other's light cones.

The metric components obviously depend on the chosen local coordinate system. Under a change of coordinates ${\displaystyle x^{\mu }\to x^{\bar {\mu }}}$  the metric components transform as

${\displaystyle g_{{\bar {\mu }}{\bar {\nu }}}={\frac {\partial x^{\rho }}{\partial x^{\bar {\mu }}}}{\frac {\partial x^{\sigma }}{\partial x^{\bar {\nu }}}}g_{\rho \sigma }=\Lambda ^{\rho }{}_{\bar {\mu }}\,\Lambda ^{\sigma }{}_{\bar {\nu }}\,g_{\rho \sigma }.}$ 

Examples

Flat spacetime

The simplest example of a Lorentzian manifold is flat spacetime which can be given as R⁴ with coordinates ${\displaystyle (t,x,y,z)}$  and the metric

${\displaystyle ds^{2}=-dt^{2}+dx^{2}+dy^{2}+dz^{2}.\,}$ 

Note that these coordinates actually cover all of R⁴. The flat space metric (or Minkowski metric) is often denoted by the symbol η. In the above coordinates, the matrix representation of η is

${\displaystyle \eta ={\begin{bmatrix}-1&0&0&0\\0&1&0&0\\0&0&1&0\\0&0&0&1\end{bmatrix}}}$ 

In spherical coordinates ${\displaystyle (t,r,\theta ,\phi )}$ , the flat space metric takes the form

${\displaystyle ds^{2}=-dt^{2}+dr^{2}+r^{2}d\Omega ^{2}\,}$ 

where

${\displaystyle d\Omega ^{2}=d\theta ^{2}+\sin ^{2}\theta \,d\phi ^{2}}$ 

is the standard metric on the 2-sphere (i.e. the standard element of solid angle).

Schwarzschild metric

Besides the flat space metric the most important metric in general relativity is the Schwarzschild metric which can be given in one set of local coordinates by

${\displaystyle ds^{2}=-\left(1-{\frac {2GM}{r}}\right)dt^{2}+\left(1-{\frac {2GM}{r}}\right)^{-1}dr^{2}+r^{2}d\Omega ^{2}}$ 

where, again, ${\displaystyle d\Omega ^{2}}$  is the standard metric on the 2-sphere. Here G is the gravitation constant and M is a constant with the dimensions of mass.

Curvature

The metric ${\displaystyle g}$  completely determines the curvature of spacetime. According to the fundamental theorem of Riemannian geometry, there is a unique connection ∇ on any Lorentzian manifold that is compatible with the metric and torsion-free. This connection is called the Levi-Civita connection. The Christoffel symbols of this connection are given in local coordinates ${\displaystyle x^{\mu }}$  by the formula

${\displaystyle \Gamma _{\mu \nu }^{\lambda }={\frac {1}{2}}g^{\lambda \rho }(\partial _{\mu }g_{\nu \rho }+\partial _{\nu }g_{\rho \mu }-\partial _{\rho }g_{\mu \nu })}$ 

The curvature of spacetime is then given by the Riemann curvature tensor which is defined in terms of the Levi-Civita connection ∇. In local coordinates this tensor is given by:

${\displaystyle {R^{\rho }}_{\sigma \mu \nu }=\partial _{\mu }\Gamma _{\nu \sigma }^{\rho }-\partial _{\nu }\Gamma _{\mu \sigma }^{\rho }+\Gamma _{\mu \lambda }^{\rho }\Gamma _{\nu \sigma }^{\lambda }-\Gamma _{\nu \lambda }^{\rho }\Gamma _{\mu \sigma }^{\lambda }.}$ 

The curvature is then expressible purely in terms of the metric ${\displaystyle g}$  and its derivatives.

Einstein's equations

One of the core ideas of general relativity is that the metric (and the associated geometry of spacetime) is determined by the matter and energy content of spacetime. Einstein's famous field equations:

${\displaystyle R_{\mu \nu }-{1 \over 2}Rg_{\mu \nu }=8\pi G\,T_{\mu \nu }}$ 

relate the metric (and the associated curvature tensors) to the energy-momentum tensor ${\displaystyle T_{\mu \nu }}$ . This equation is a complicated set of nonlinear partial differential equations for the metric components. Exact solutions of this equation are very difficult to come by; see exact solutions of Einstein's field equations for more information.