Hamiltonian Cosmological Perturbation Theory
Abstract
The Hamiltonian approach to cosmological perturbations in general relativity in finite space-time is developed, where a cosmological scale factor is identified with spatial averaging the metric determinant logarithm. This identification preserves the number of variables and leads to a cosmological perturbation theory with the scalar potential perturbations in contrast to the kinetic perturbations in the Lifshitz version which are responsible for the ``primordial power spectrum'' of CMB in the inflationary model. The Hamiltonian approach enables to explain this ``spectrum'' in terms of scale-invariant variables and to consider other topical problem of modern cosmology in the context of quantum cosmological creation of both universes and particles from the stable Bogoliubov vacuum.
Keywords
Cite
@article{arxiv.hep-th/0501242,
title = {Hamiltonian Cosmological Perturbation Theory},
author = {B. M. Barbashov and V. N. Pervushin and A. F. Zakharov and V. A. Zinchuk},
journal= {arXiv preprint arXiv:hep-th/0501242},
year = {2009}
}
Comments
10 pages, text was changed according to the version accepted for publication in Physics Letters B