Hamiltonian Cosmological Perturbation Theory
arXiv:hep-th/0501242 · doi:10.1016/j.physletb.2005.12.024
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.
10 pages, text was changed according to the version accepted for publication in Physics Letters B
References in corpus (6)
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- Measurements of Omega and Lambda from 42 High-Redshift Supernovae
- Scalar-tensor gravity in an accelerating universe
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