Causal propagation of geometrical fields in relativistic cosmology

Details Causal propagation of geometrical fields in relativistic cosmology Causal propagation of geometrical fields in relativistic cosmology

1998-10-18

arxiv.org/abs/gr-qc/9810058v1

Phys.Rev. D59 (1999) 024013

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

25 pages, RevTeX (10pt), accepted for publication by Physical Review D

Scientific paper

10.1103/PhysRevD.59.024013

We employ the extended 1+3 orthonormal frame formalism for fluid spacetime geometries $({\cal M}, {\bf g}, {\bf u})$, which contains the Bianchi field equations for the Weyl curvature, to derive a 44-D evolution system of first-order symmetric hyperbolic form for a set of geometrically defined dynamical field variables. Describing the matter source fields phenomenologically in terms of a barotropic perfect fluid, the propagation velocities $v$ (with respect to matter-comoving observers that Fermi-propagate their spatial reference frames) of disturbances in the matter and the gravitational field, represented as wavefronts by the characteristic 3-surfaces of the system, are obtained. In particular, the Weyl curvature is found to account for two (non-Lorentz-invariant) Coulomb-like characteristic eigenfields propagating with $v = 0$ and four transverse characteristic eigenfields propagating with $|v| = 1$, which are well known, and four (non-Lorentz-invariant) longitudinal characteristic eigenfields propagating with $|v| = \sfrac{1}{2}$. The implications of this result are discussed in some detail and a parallel is drawn to the propagation of irregularities in the matter distribution. In a worked example, we specialise the equations to cosmological models in locally rotationally symmetric class II and include the constraints into the set of causally propagating dynamical variables.

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