Flat deformation theorem and symmetries in spacetime

Details Flat deformation theorem and symmetries in spacetime Flat deformation theorem and symmetries in spacetime

2008-09-05

arxiv.org/abs/0809.1030v3

Class.Quant.Grav.26:055013,2009

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

30 pages, 0 figures

Scientific paper

10.1088/0264-9381/26/5/055013

The \emph{flat deformation theorem} states that given a semi-Riemannian analytic metric $g$ on a manifold, locally there always exists a two-form $F$, a scalar function $c$, and an arbitrarily prescribed scalar constraint depending on the point $x$ of the manifold and on $F$ and $c$, say $\Psi (c, F, x)=0$, such that the \emph{deformed metric} $\eta = cg -\epsilon F^2$ is semi-Riemannian and flat. In this paper we first show that the above result implies that every (Lorentzian analytic) metric $g$ may be written in the \emph{extended Kerr-Schild form}, namely $\eta_{ab} := a g_{ab} - 2 b k_{(a} l_{b)}$ where $\eta$ is flat and $k_a, l_a$ are two null covectors such that $k_a l^a= -1$; next we show how the symmetries of $g$ are connected to those of $\eta$, more precisely; we show that if the original metric $g$ admits a Conformal Killing vector (including Killing vectors and homotheties), then the deformation may be carried out in a way such that the flat deformed metric $\eta$ `inherits' that symmetry.

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