# Pseudo-Riemannian space

A space with an affine connection (without torsion), at each point of which the tangent space is a pseudo-Euclidean space.

Let $ A _ {n} $ be an $ n $- space with an affine connection (without torsion) and let $ {} ^ {l} \mathbf R _ {n} $ be the tangent pseudo-Euclidean space at every point of $ A _ {n} $; in this case the pseudo-Riemannian space is denoted by $ {} ^ {l} V _ {n} $. As in a proper Riemannian space the metric tensor of $ {} ^ {l} V _ {n} $ is non-degenerate, has vanishing covariant derivative, but the metric form of $ {} ^ {l} V _ {n} $ is a quadratic form of index $ l $:

$$ d s ^ {2} = g _ {ij} d x ^ {i} d x ^ {j} ,\ \ i , j = 1 \dots n , $$

$ g _ {ij} $ is the metric tensor of $ {} ^ {l} V _ {n} $, $ \mathop{\rm det} \| g _ {ij} \| \neq 0 $. The space $ {} ^ {l} V _ {n} $ can be defined as an $ n $- dimensional manifold on which an invariant quadratic differential form of index $ l $ is given.

The simplest example of a pseudo-Riemannian space is the space $ {} ^ {l} \mathbf R _ {n} $.

The pseudo-Riemannian space $ {} ^ {l} V _ {n} $ is said to be reducible if in a neighbourhood of each point there is a system of coordinates $ ( x ^ {1} \dots x ^ {n} ) $ such that the coordinates $ x ^ {i} $ can all be separated into groups $ x ^ {i _ \alpha } $ such that $ g _ {i _ \alpha j _ \alpha } \neq 0 $ only for those indices $ i _ \alpha $ and $ j _ \alpha $ which belong to a single group and the $ g _ {i _ \alpha j _ \alpha } $ are functions only of the coordinates of this group.

In a pseudo-Riemannian space the sectional curvature is defined for every non-degenerate two-dimensional direction. It can be interpreted as the curvature of the geodesic (non-isotropic) $ 2 $- surface drawn through the given point in the given two-dimensional direction. If the value of the curvature at each point is the same for all two-dimensional directions, then it is constant at all points (Schur's theorem), and in this case the space is said to be a pseudo-Riemannian space of constant curvature $ ( n \geq 3 ) $. An example of a pseudo-Riemannian space of constant negative curvature is the hyperbolic space $ {} ^ {l} S _ {n} $ of negative curvature — it is a pseudo-Riemannian space $ {} ^ {n-} l V _ {n} $; the space $ {} ^ {l} \mathbf R _ {n} $ is a pseudo-Riemannian space of vanishing curvature.

#### References

[1] | P.K. [P.K. Rashevskii] Rashewski, "Riemannsche Geometrie und Tensoranalyse" , Deutsch. Verlag Wissenschaft. (1959) (Translated from Russian) |

[2] | B.A. Rozenfel'd, "Non-Euclidean spaces" , Moscow (1969) (In Russian) Zbl 0767.53035 Zbl 0713.53012 Zbl 0702.53009 |

[3] | A. Einstein, "Collected scientific works" , 1 , Moscow (1965) (In Russian; translated from English) |

#### Comments

Important for applications in physics is the case of index 1. For any $ n $, $ {} ^ {1} V _ {n} $ is called a Lorentzian manifold. Here the tangent vectors having purely imaginary, vanishing or non-vanishing real length are called time-like, light-like or space-like, respectively. If $ n = 4 $ and $ {} ^ {1} V _ {n} $ possesses a global time-like vector field, then $ {} ^ {1} V _ {n} $ is called a space-time and admits a distinction between future and past. Such a space-time is the general geometric model in which the phenomena of the theory of general relativity are described. For example, the history of a material or light-like particle is described by a world-line having non-space-like tangents only. The coupling between the geometric model and the physical data is given by Einstein's field equations (cf. Einstein equations).

During the last decades much progress has been made concerning global Lorentzian geometry. This was initiated by R. Penrose and pursued by S.W. Hawking in particular (see [a2]). The main highlights in this development are the Hawking–Penrose singularity theorems, showing that under special geometric conditions (e.g. non-negative Ricci curvature in time-like directions and the existence of a compact space-like hypersurface with positive mean curvature, or non-negative Ricci curvature in light-like directions and the existence of a non-compact Cauchy hypersurface and a trapped surface) the space-time has a future singularity, i.e. there exists a future-incomplete, causal geodesic. Up to time orientation the standard models for these singularities are the Schwarzschild model (black hole) and the Robertson–Walker–Friedman model (big-bang). See also Cosmological models. The corresponding theory can be found in [a1]–[a4].

#### References

[a1] | J.K. Beem, P.E. Ehrlich, "Global Lorentzian geometry" , M. Dekker (1981) MR0619853 Zbl 0462.53001 |

[a2] | S.W. Hawking, G.F.R. Ellis, "The large scale structure of space-time" , Cambridge Univ. Press (1973) MR0424186 Zbl 0265.53054 |

[a3] | B. O'Neill, "Semi-Riemannian geometry (with applications to relativity)" , Acad. Press (1983) |

[a4] | R.K. Sachs, H. Wu, "General relativity for mathematicians" , Springer (1977) MR0503498 MR0503499 Zbl 0373.53001 |

[a5] | C.W. Misner, K.S. Thorne, J.A. Wheeler, "Gravitation" , Freeman (1973) MR0418833 Zbl 1177.83013 Zbl 0078.19106 |

**How to Cite This Entry:**

Pseudo-Riemannian space.

*Encyclopedia of Mathematics.*URL: http://encyclopediaofmath.org/index.php?title=Pseudo-Riemannian_space&oldid=48343