Stochastic Properties of Cosmological Perturbations

  • Oliver PiattellaEmail author
Part of the UNITEXT for Physics book series (UNITEXTPH)


The attentive reader must have noticed that, in fact, we have given no actual initial conditions on cosmological perturbations in Chap. 6. What we have done is to give the form of the primordial modes and show how, in the 5 different cases that we investigated, all scalar perturbations are sourced by a single scalar potential. For example, in the adiabatic case we showed in Eq.  6.77 how \(\Phi (\mathbf k)\) is related to \(C_\gamma (\mathbf k)\), which we proved to be equal to \(\zeta (\mathbf k)\) and \(\mathcal R(\mathbf k)\).


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© Springer International Publishing AG, part of Springer Nature 2018

Authors and Affiliations

  1. 1.Núcleo Cosmo-UFES and Department of PhysicsFederal University of Espírito SantoVitóriaBrazil

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