No data available.

Please log in to see this content.

You have no subscription access to this content.

No metrics data to plot.

The attempt to load metrics for this article has failed.

The attempt to plot a graph for these metrics has failed.

The full text of this article is not currently available.

Symmetries and metrics of homogeneous cosmologies

### Abstract

It is shown that an assumption of ’’historical homogeneity’’—or the persistence of spatial homogeneity in time—leads to the synchronous (time‐orthogonal) form d*s* ^{2}=−d*t* ^{2}+γ_{ A B } (*t*)ε^{ A }⊗ε^{ B }, of the metrics for general spatially homogeneous (Bianchi) cosmologies. The ε^{ A } are group‐representation 1‐forms associated with the spatial symmetry group of the given cosmology, and are independent of any particular space–time theory; in particular they do not depend on Einstein’s equations and the local physics. Expressions for the ε^{ A } in the canonical basis used by Estabrook, Wahlquist, and Behr (EWB) have been tabulated in the companion paper on ’’Spatially homogeneous neutrino cosmologies’’ (SHNC). In the present paper explicit expressions are given for the scale factors γ_{ A B }(*t*). These do correspond to the choice of the canonical basis to describe the symmetry but, in contrast to the ε^{ A }, they also depend on the space–time physical theory. Here the γ_{ A B }(*t*) come out as observable geometric–kinematic quantities (generalized Hubble constants) which also appear in the solutions of Einstein’s equations for a given cosmology. Central to the discussion is the matrix C(*t*) which relates the time‐independent canonical basis describing the symmetry to a time‐dependent orthonormalizing basis. With the imposed requirement that the Riemannian geometry of the evolving spatial hypersurfaces retain its quasi‐canonical form in time (’’quasi‐canonical gauge’’) it is shown that C(*t*) is a product of a diagonal matrix D̀ and a rotation matrix R; and a table of these forms of C(*t*) for the various Bianchi types is given. The simple Hubble‐constant expressions for the metric scale factors γ_{ A B }(*t*) for all types come solely from the diagonal factor D̀ in C. The metric, then, in all cases takes the form d*s* ^{2}=−d*t* ^{2}+γ_{ A B }ε^{ A } ⊗ε^{ B }=−d*t* ^{2} +(ε^{I}/α)^{2} +(ε^{II}/β)^{2} +(ε^{III}/γ)^{2}. Thus, the specializing assumption of Misner and of Ryan and Shepley, requiring C to be symmetric, does not limit the form of the metric but does restrict the relation between the invariant symmetry basis and the quasi‐canonical orthonormal basis to the cases where the orthogonal factor R reduces to the identity, i.e., to those cases where the two bases remain parallel at all times. Thus, the gauge assumed by them is not compatible with the preservation of the quasi‐canonical form of the spatial geometry in almost all cases where there is degeneracy involved in the spatial curvatures.

© 1980 American Institute of Physics

Published online 21 July 2008

/content/aip/journal/jmp/21/7/10.1063/1.524612

http://aip.metastore.ingenta.com/content/aip/journal/jmp/21/7/10.1063/1.524612

Article metrics loading...

/content/aip/journal/jmp/21/7/10.1063/1.524612

2008-07-21

2016-09-28

Full text loading...

###
Most read this month

Article

content/aip/journal/jmp

Journal

5

3

Commenting has been disabled for this content