Scalar and Vector Perturbations in Quantum Cosmological Backgrounds

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dc.creatorPinho, Emanuel J. C.
dc.creatorPinto-Neto, Nelson
dc.date2006-10-17
dc.date.accessioned2026-07-07T11:28:01Z
dc.date.available2026-07-07T11:28:01Z
dc.descriptionGeneralizing a previous work concerning cosmological linear tensor perturbations, we show that the lagrangians and hamiltonians of cosmological linear scalar and vector perturbations can be put in simple form through the implementation of canonical transformations and redefinitions of the lapse function, without ever using the background classical equations of motion. In particular, if the matter content of the Universe is a perfect fluid, the hamiltonian of scalar perturbations can be reduced, as usual, to a hamiltonian of a scalar field with variable mass depending on background functions, independently of the fact that these functions satisfy the background Einstein's classical equations. These simple lagrangians and hamiltonians can then be used in situations where the background metric is also quantized, hence providing a substantial simplification over the direct approach originally developed by Halliwell and Hawking.
dc.description19 pages, no figure
dc.identifierhttps://arxiv.org/abs/hep-th/0610192
dc.identifierhttp://arxiv.org/abs/hep-th/0610192
dc.identifierPhys.Rev.D76:023506,2007
dc.identifierdoi:10.1103/PhysRevD.76.023506
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/196312
dc.subjectHigh Energy Physics - Theory
dc.titleScalar and Vector Perturbations in Quantum Cosmological Backgrounds
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