Stochastic semiclassical equations for weakly inhomogeneous cosmologies

Details Stochastic semiclassical equations for weakly inhomogeneous cosmologies Stochastic semiclassical equations for weakly inhomogeneous cosmologies

1995-11-28

arxiv.org/abs/gr-qc/9511078v1

Phys.Rev. D53 (1996) 1927-1937

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

20 pages, LaTeX (RevTeX). A postscript version is available at ftp://ftp.ifae.es/preprint/ft/uabft373.ps

Scientific paper

10.1103/PhysRevD.53.1927

Semiclassical Einstein-Langevin equations for arbitrary small metric perturbations conformally coupled to a massless quantum scalar field in a spatially flat cosmological background are derived. Use is made of the fact that for this problem the in-in or closed time path effective action is simply related to the Feynman and Vernon influence functional which describes the effect of the ``environment'', the quantum field which is coarse grained here, on the ``system'', the gravitational field which is the field of interest. This leads to identify the dissipation and noise kernels in the in-in effective action, and to derive a fluctuation-dissipation relation. A tensorial Gaussian stochastic source which couples to the Weyl tensor of the spacetime metric is seen to modify the usual semiclassical equations which can be viewed now as mean field equations. As a simple application we derive the correlation functions of the stochastic metric fluctuations produced in a flat spacetime with small metric perturbations due to the quantum fluctuations of the matter field coupled to these perturbations.

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