Rotating and twisting locally rotationally symmetric spacetimes: a general solution

Abstract

In this paper we derive a general solution for the most general rotating and twisting locally rotationally symmetric spacetimes. This is achieved in three steps. First we decompose the manifold via 1+1+2 semi-tetrad formalism that yields a set of geometrical and thermodynamic scalars for the spacetime. We then recast the Einstein field equations in terms of evolution and propagation of these scalars. It is then shown that this class of spacetimes must possess self similarity and we use this property to solve for these scalars, thus obtaining a general solution. This solution has a number of very interesting cosmological or astrophysical consequences which we discuss in detail.

arXiv comment7 pages, Revetx 4

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Cited by in corpus (7)

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• General Perturbations of Homogeneous and Orthogonal Locally Rotationally Symmetric Class II Cosmologies with Applications to Dissipative Fluids
• Quantum Kasner transition in a locally rotationally symmetric Bianchi II universe
• Non-existence of expansion-free dynamical stars with rotation and spatial twist