Equivalence classes of perturbations in cosmologies of Bianchi types I and V: Formulation
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Publication:4270395
DOI10.1063/1.532938zbMath0952.83043OpenAlexW2090638799MaRDI QIDQ4270395
Publication date: 21 November 1999
Published in: Journal of Mathematical Physics (Search for Journal in Brave)
Full work available at URL: https://doi.org/10.1063/1.532938
perfect fluidequivalence classesquantum variablesanisotropic backgroundBianchi types I and Vexact solutions to Einstein's field equationsgauge-invariant perturbation
Relativistic cosmology (83F05) Quantization of the gravitational field (83C45) Exact solutions to problems in general relativity and gravitational theory (83C15)
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Cites Work
- Gauge-invariant cosmological perturbation theory for collisionless matter: Application to the Einstein-Liouville system
- Geometrization of linear perturbation theory for diffeomorphism-invariant covariant field equations. I: The notion of a gauge-invariant variable
- Geometrization of linear perturbation theory for diffeomorphism-invariant covariant field equations. II: Basic gauge-invariant variables with applications to de Sitter space-time
- General covariance in general relativity?
- Theory of cosmological perturbations formulated in terms of a complete set of basic gauge-invariant quantities
- Gauge-invariant perfect-fluid Robertson-Walker perturbations
- Perturbations of Friedmann-Robertson-Walker cosmological models
- Local symmetries and constraints
- Equivalence classes of perturbations in cosmologies of Bianchi types I and V: Interpretation
- Perturbation theory based on the Einstein–Boltzmann system. I. Illustration of the theory for a Robertson–Walker geometry
- Perturbation theory based on the Einstein–Boltzmann system. II. Illustration of the theory for an almost-Robertson–Walker geometry
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