Hamiltonian cosmological perturbation theory

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 p...

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Bibliographic Details
Published inPhysics letters. B Vol. 633; no. 4-5; pp. 458 - 462
Main Authors Barbashov, B.M., Pervushin, V.N., Zakharov, A.F., Zinchuk, V.A.
Format Journal Article
LanguageEnglish
Russian
Published Amsterdam Elsevier B.V 16.02.2006
Elsevier Science
Subjects
Cosmology
General relativity and gravitation
Observational cosmology
Cosmology
Observational cosmology
95.30.Sf
General relativity and gravitation
98.80.-k
98.80.Es
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Summary: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.
ISSN:0370-2693
1873-2445
DOI:10.1016/j.physletb.2005.12.024