Hamiltonian theory of classical and quantum gauge invariant perturbations in Bianchi I spacetimes
arXiv:2003.08428 · doi:10.1103/PhysRevD.101.123531
Abstract
We derive a Hamiltonian formulation of the theory of gauge invariant, linear perturbations in anisotropic Bianchi I spacetimes, and describe how to quantize this system. The matter content is assumed to be a minimally coupled scalar field with potential . We show that a Bianchi I spacetime generically induces both anisotropies and quantum entanglement on cosmological perturbations, and provide the tools to compute the details of these features. We then apply this formalism to a scenario in which the inflationary era is preceded by an anisotropic Bianchi I phase, and discuss the potential imprints in observable quantities. The formalism developed here paves the road to a simultaneous canonical quantization of both the homogeneous degrees of freedom and the perturbations, a task that we develop in a companion paper.
arXiv commentv1: 41 pages, 3 figures; v2 : 42 pages, 4 figures, minor changes, one figure and references added, version published in Phys. Rev. D
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- Observational consequences of Bianchi I spacetimes in loop quantum cosmology
- QFT in Curved Spacetime from Quantum Gravity: proper WKB decomposition of the gravitational component
- Loop quantum cosmology: relation between theory and observations
- Classical and quantum field theory in a box with moving boundaries: A numerical study of the Dynamical Casimir Effect
- Observational constraints on anisotropies for bouncing alternatives to inflation
- Polar perturbations in Kantowski-Sachs spacetimes and hybrid quantum cosmology
- xAct Implementation of the Theory of Cosmological Perturbation in Bianchi I Spacetimes
- Dirac procedure and the Hamiltonian formalism for cosmological perturbations in a Bianchi I universe
- Gauge-fixing and spacetime reconstruction in the Hamiltonian theory of cosmological perturbations
- Quantum geometric formulation of Brans-Dicke theory for Bianchi I spacetime
- Inflation from inhomogeneous polarized Gowdy model