After using the previous decomposition, the noise kernel defined in Equation (12) can be written as

where we have used the fact that for Gaussian states on the background geometry. We consider the vacuum state to be the Euclidean vacuum, which is Gaussian and is the preferred state in the de Sitter background. In the above equation the first term is quadratic in , whereas the second one is quartic. Both contributions to the noise kernel are separately conserved, since both and satisfy the Klein–Gordon field equations on the background spacetime. Consequently, the two terms can be considered separately. On the other hand, if one treats as a small perturbation the second term in (171) is of lower order than the first and may be consistently neglected. This corresponds to neglecting the last term of Equation (169). The stress tensor fluctuations due to a term of that kind were considered in [314].We can now write down the Einstein–Langevin equations (167) to linear order in the inflaton fluctuations. It is easy to check [316] that the space-space components coming from the stress-tensor expectation-value terms and the stochastic tensor are diagonal, i.e., for . This, in turn, implies that the two functions characterizing the scalar metric perturbations are equal: in agreement with [270]. The equation for can be obtained from the -component of the Einstein–Langevin equation, which, neglecting a nonlocal term, reads in Fourier space as,

where is the comoving momentum component associated to the comoving coordinate , and we have used the definition . Here primes denote derivatives with respect to the conformal time and . A nonlocal term of dissipative character, which comes from the second term in Equation (169), should also appear on the left-hand side of Equation (172), but we have neglected it to simplify the forthcoming expressions (the large scale spectrum does not change in a substantial way). We must emphasize, however, that the proof of the equivalence of the stochastic approach to linear order in to the usual linear cosmological perturbations approach does not assume that simplification [316]. To solve Equation (172), whose left-hand side comes from the linearized Einstein tensor for the perturbed metric [270], we need the retarded propagator for the gravitational potential , where is a homogeneous solution of Equation (172) related to the initial conditions chosen and . For instance, if we take , the solution would correspond to “turning on” the stochastic source at . With the solution of the Einstein–Langevin equation (172) for the scalar metric perturbations we are in position to compute the two-point correlation functions for these perturbations.http://www.livingreviews.org/lrr-2008-3 |
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