I M Khalatnikov et al JCAP03(2003)001 doi:10.1088/1475-7516/2003/03/001
Quasi-isotropic solution of the Einstein equations near a cosmological singularity for a two-fluid cosmological model
I M Khalatnikov1,2,3, A Yu Kamenshchik1,2, M Martellini2,4,5 and A A Starobinsky1
Show affiliationsThe quasi-isotropic inhomogeneous solution of the Einstein equations near a cosmological singularity in the form of a series expansion in the synchronous system of reference, first found by Lifshitz and Khalatnikov in 1960, is generalized to the case of a two-fluid cosmological model. This solution describes non-decreasing modes of adiabatic and isocurvature scalar perturbations and gravitational waves in the regime when deviations of a spacetime metric from the homogeneous isotropic Friedmann–Robertson–Walker (FRW) background are large while locally measurable quantities like Riemann tensor components are still close to their FRW values. The general structure of the perturbation series is presented and the first coefficients of the series expansion for the metric tensor and the fluid energy densities and velocities are calculated explicitly.
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Issue 03 (March 2003)
Received 25 January 2003, accepted for publication 17 February 2003
Published 4 March 2003
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Quasi-isotropic solution of the Einstein equations near a cosmological singularity for a two-fluid cosmological model
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