Metric tensor (general relativity)
Metric tensor of spacetime in
general relativity written as a matrix
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 potential of Newtonian gravitation. The metric captures all the geometric and causal structure of spacetime, being used to define notions such as time, distance, volume, curvature, angle, and separating the future and the past.
Notation and conventions
Throughout this article we work with a metric signature that is mostly positive (− + + +); see sign convention. The gravitation constant G will be kept explicit. The summation convention, where repeated indices are automatically summed over, is employed.
Mathematically, spacetime is represented by a 4-dimensional differentiable manifold M and the metric is given as a covariant, second-order, 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 a type of 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 at a point x in M, the metric can be evaluated on u and v to give a real number:
This can be thought of as a generalization of the dot product in ordinary Euclidean space. This analogy is not exact, however. Unlike 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
The factors are one-form gradients of the scalar coordinate fields . The metric is thus a linear combination of tensor products of one-form gradients of coordinates. The coefficients are a set of 16 real-valued functions (since the tensor g is a tensor field, which is defined at all points of a spacetime manifold). In order for the metric to be symmetric we must have
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 . The nondegeneracy of 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 themselves as the metric (see, however, abstract index notation).
With the quantities being regarded as the components of an infinitesimal coordinate displacement four-vector (not to confused with the one-forms of the same notation above), the metric determines the invariant square of an infinitesimal line element, often referred to as an interval. The interval is often denoted
The interval imparts information about the causal structure of spacetime. When , 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 traversed by a massive object. When , the interval is lightlike, and can only be traversed by light. When , the interval is spacelike and the square root of ds2 acts as an incremental proper length. Spacelike intervals cannot be traversed, since they connect events that are outside each other's light cones. Events can be causally related only if they are within each other's light cones.
The components of the metric depend on the choice of local coordinate system. Under a change of coordinates , the metric components transform as
The simplest example of a Lorentzian manifold is flat spacetime, which can be given as R4 with coordinates and the metric
Note that these coordinates actually cover all of R4. The flat space metric (or Minkowski metric) is often denoted by the symbol η and is the metric used in special relativity. In the above coordinates, the matrix representation of η is
(An alternative convention replaces coordinate t by ct, and defines η as in Minkowski space § Standard basis.)
In spherical coordinates , the flat space metric takes the form
is the standard metric on the 2-sphere.
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
where, again, is the standard metric on the 2-sphere. Here G is the gravitation constant and M is a constant with the dimensions of mass. Its derivation can be found here. The Schwarzschild metric approaches the Minkowski metric as M approaches zero (except at the origin where it is undefined). Similarly, when r goes to infinity, the Schwarzschild metric approaches the Minkowski metric.
Other notable metrics are:
- Alcubierre metric,
- de Sitter/anti-de Sitter metrics,
- Eddington–Finkelstein coordinates,
- Friedmann–Lemaître–Robertson–Walker metric,
- Gullstrand–Painlevé coordinates,
- Isotropic coordinates,
- Kerr metric,
- Kerr–Newman metric,
- Kruskal–Szekeres coordinates,
- Lemaître coordinates,
- Lemaître–Tolman metric (aka Bondi metric),
- Peres metric,
- Reissner–Nordström metric,
- Rindler coordinates,
- Weyl−Lewis−Papapetrou coordinates.
where det[gμν] is the determinant of the matrix of components of the metric tensor for the given coordinate system.
The metric g completely determines the curvature of spacetime. According to the fundamental theorem of Riemannian geometry, there is a unique connection ∇ on any semi-Riemannian 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 terms of partial derivatives of the metric in local coordinates by the formula
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:
The curvature is then expressible purely in terms of the metric and its derivatives.
where the Ricci curvature tensor
and the scalar curvature
relate the metric (and the associated curvature tensors) to the stress–energy tensor . This tensor equation is a complicated set of nonlinear partial differential equations for the metric components. Exact solutions of Einstein's field equations are very difficult to find.
- Alternatives to general relativity
- Basic introduction to the mathematics of curved spacetime
- Mathematics of general relativity
- Ricci calculus
See general relativity resources for a list of references.