Misplaced Pages

Part of a series on
Spacetime
Special relativity General relativity
Spacetime concepts Spacetime manifold Equivalence principle Lorentz transformations Minkowski space
General relativity Introduction to general relativity Mathematics of general relativity Einstein field equations
Classical gravity Introduction to gravitation Newton's law of universal gravitation
Relevant mathematics Four-vector Derivations of relativity Spacetime diagrams Differential geometry Curved space Curved spacetime Mathematics of general relativity Spacetime topology
Physics portal  Category
v t e

Spacetime topology is the topological structure of spacetime, a topic studied primarily in general relativity. This physical theory models gravitation as the curvature of a four dimensional Lorentzian manifold (a spacetime) and the concepts of topology thus become important in analysing local as well as global aspects of spacetime. The study of spacetime topology is especially important in physical cosmology.

Types of topology

There are two main types of topology for a spacetime M.

Manifold topology

As with any manifold, a spacetime possesses a natural manifold topology. Here the open sets are the image of open sets in ${\displaystyle \mathbb {R} ^{4}}$.

Path or Zeeman topology

Definition: The topology ${\displaystyle \rho }$ in which a subset ${\displaystyle E\subset M}$ is open if for every timelike curve ${\displaystyle c}$ there is a set ${\displaystyle O}$ in the manifold topology such that ${\displaystyle E\cap c=O\cap c}$.

It is the finest topology which induces the same topology as ${\displaystyle M}$ does on timelike curves.

Properties

Strictly finer than the manifold topology. It is therefore Hausdorff, separable but not locally compact.

A base for the topology is sets of the form ${\displaystyle Y^{+}(p,U)\cup Y^{-}(p,U)\cup p}$ for some point ${\displaystyle p\in M}$ and some convex normal neighbourhood ${\displaystyle U\subset M}$.

(${\displaystyle Y^{\pm }}$ denote the chronological past and future).

Alexandrov topology

The Alexandrov topology on spacetime, is the coarsest topology such that both ${\displaystyle Y^{+}(E)}$ and ${\displaystyle Y^{-}(E)}$ are open for all subsets ${\displaystyle E\subset M}$.

Here the base of open sets for the topology are sets of the form ${\displaystyle Y^{+}(x)\cap Y^{-}(y)}$ for some points ${\displaystyle \,x,y\in M}$.

This topology coincides with the manifold topology if and only if the manifold is strongly causal but it is coarser in general.

Note that in mathematics, an Alexandrov topology on a partial order is usually taken to be the coarsest topology in which only the upper sets ${\displaystyle Y^{+}(E)}$ are required to be open. This topology goes back to Pavel Alexandrov.

Nowadays, the correct mathematical term for the Alexandrov topology on spacetime (which goes back to Alexandr D. Alexandrov) would be the interval topology, but when Kronheimer and Penrose introduced the term this difference in nomenclature was not as clear, and in physics the term Alexandrov topology remains in use.

Planar spacetime

Events connected by light have zero separation. The plenum of spacetime in the plane is split into four quadrants, each of which has the topology of R. The dividing lines are the trajectory of inbound and outbound photons at (0,0). The planar-cosmology topological segmentation is the future F, the past P, space left L, and space right D. The homeomorphism of F with R amounts to polar decomposition of split-complex numbers:

${\displaystyle z=\exp(a+jb)=e^{a}(\cosh b+j\sinh b)\to (a,b),}$ so that

${\displaystyle z\to (a,b)}$ is the split-complex logarithm and the required homeomorphism F → R, Note that b is the rapidity parameter for relative motion in F.

F is in bijective correspondence with each of P, L, and D under the mappings z → –z, z → jz, and z → – j z, so each acquires the same topology. The union U = F ∪ P ∪ L ∪ D then has a topology nearly covering the plane, leaving out only the null cone on (0,0). Hyperbolic rotation of the plane does not mingle the quadrants, in fact, each one is an invariant set under the unit hyperbola group.

See also

• 4-manifold
• Clifford-Klein form
• Closed timelike curve
• Complex spacetime
• Geometrodynamics
• Gravitational singularity
• Hantzsche-Wendt manifold
• Spacetime curvature
• Wormhole

Notes

1. Luca Bombelli website Archived 2010-06-16 at the Wayback Machine
2. *Zeeman, E.C. (1967). "The topology of Minkowski space". Topology. 6 (2): 161–170. doi:10.1016/0040-9383(67)90033-X.
3. Penrose, Roger (1972), Techniques of Differential Topology in Relativity, CBMS-NSF Regional Conference Series in Applied Mathematics, p. 34

References

• Zeeman, E. C. (1964). "Causality Implies the Lorentz Group". Journal of Mathematical Physics. 5 (4): 490–493. Bibcode:1964JMP.....5..490Z. doi:10.1063/1.1704140.
• Hawking, S. W.; King, A. R.; McCarthy, P. J. (1976). "A new topology for curved space–time which incorporates the causal, differential, and conformal structures" (PDF). Journal of Mathematical Physics. 17 (2): 174–181. Bibcode:1976JMP....17..174H. doi:10.1063/1.522874.

• General relativity
• Lorentzian manifolds