Scalar and Vector Perturbations in Quantum Cosmological Backgrounds

Details Scalar and Vector Perturbations in Quantum Cosmological Backgrounds Scalar and Vector Perturbations in Quantum Cosmological Backgrounds

2006-10-17

arxiv.org/abs/hep-th/0610192v1

Phys.Rev.D76:023506,2007

Physics

High Energy Physics

High Energy Physics - Theory

19 pages, no figure

Scientific paper

10.1103/PhysRevD.76.023506

Generalizing 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.

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