Gaugeinvariant cosmological perturbations
Abstract
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 gaugeinvariant 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 nongaugeinvariant perturbation in the density itself is illdefined. 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.
 Publication:

Physical Review D
 Pub Date:
 October 1980
 DOI:
 10.1103/PhysRevD.22.1882
 Bibcode:
 1980PhRvD..22.1882B