Quantization of perturbations during inflation in the 1+3 covariant formalism
arXiv:gr-qc/0701121 · doi:10.1103/PhysRevD.75.087302
Abstract
This note derives the analogue of the Mukhanov-Sasaki variables both for scalar and tensor perturbations in the 1+3 covariant formalism. The possibility of generalizing them to non-flat Friedmann-Lemaitre universes is discussed.
arXiv comment4 pages: v2 has minor changes to match published version
References in corpus (12)
- Non-Gaussian features of primordial fluctuations in single field inflationary models
- Cosmological perturbations in a generalized gravity including tachyonic condensation
- Conserved non-linear quantities in cosmology
- Evolution of non-linear cosmological perturbations
- Parametric amplification of metric fluctuations through a bouncing phase
- WMAP data and the curvature of space
- Canonical Quantization of Cosmological Perturbations in the One Bubble Open Universe
- Nonlinear perturbations of cosmological scalar fields
- Gravitational waves generated by second order effects during inflation
- Evolution of the Bianchi I, the Bianchi III and the Kantowski-Sachs Universe: Isotropization and Inflation
- Dynamics of Inflationary Universes with Positive Spatial Curvature
- Cosmological density fluctuations and gravity waves: A covariant approach to gauge-invariant non-linear perturbation theory
Cited by in corpus (8)
- Relativistic cosmology and large-scale structure
- Theory of cosmological perturbations in an anisotropic universe
- Predictions from an anisotropic inflationary era
- The radiative transfer at second order: a full treatment of the Boltzmann equation with polarization
- Conserved cosmological perturbation in Galileon models
- A geometrical approach to nonlinear perturbations in relativistic cosmology
- Gauge invariant Boltzmann equation and the fluid limit
- Second order Boltzmann equation : gauge dependence and gauge invariance