Gauge-invariant cosmological perturbations

Journal Article · Wed Oct 15 04:00:00 EDT 1980 · Phys. Rev., D; (United States)

DOI:https://doi.org/10.1103/PhysRevD.22.1882· OSTI ID:5003202

Bardeen, J M

The physical interpretation of perturbations of homogeneous, isotropic cosmological models in the early Universe, when the perturbation is larger than the particle horizon, is clarified by defining a complete set of gauge-invariant variables. The linearized perturbation equations written in these variables are simpler than the usual versions, and easily accommodate an arbitrary background equation of state, entropy perturbations, and anisotropic pressure perturbations. Particular attention is paid to how a scalar (density) perturbation might be generated by stress perturbations at very early times, when the non-gauge-invariant perturbation in the density itself is ill-defined. The amplitude of the fractional energy density perturbation at the particle horizon cannot be larger, in order of magnitude, than the maximum ratio of the stress perturbation to the background energy density at any earlier time, unless the perturbation is inherent in the initial singularity.

• Research Organization: Institute for Advanced Study, Princeton, New Jersey 08540
• OSTI ID: 5003202
• Journal Information: Phys. Rev., D; (United States), Journal Name: Phys. Rev., D; (United States) Vol. 22:8; ISSN PRVDA
• Country of Publication: United States
• Language: English

Related Subjects

640106* -- Astrophysics & Cosmology-- Cosmology
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
COSMOLOGICAL MODELS
DISTURBANCES
ENTROPY
EQUATIONS
EQUATIONS OF STATE
GAUGE INVARIANCE
INVARIANCE PRINCIPLES
MATHEMATICAL MODELS
METRICS
PERTURBATION THEORY
PHYSICAL PROPERTIES
SPACE-TIME
THERMODYNAMIC PROPERTIES
TIME DEPENDENCE
UNIVERSE