Cosmological perturbation theory

By R. Durrer. 2004

537 citations recorded by the source corpus.

This is a review on cosmological perturbation theory. After an introduction, it presents the problem of gauge transformation. Gauge invariant variables are introduced and the Einstein and conservation equations are written in terms of these variables. Some examples, especially perfect fluids and scalar fields are presented in detail. The generation of perturbations during inflation is studied. Lightlike geodesics and their relevance for CMB anisotropies are briefly discussed. Perturbation theory in braneworlds is also introduced.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1f32e6b2e00fddc5cf9aa642e0b733e6b37e600e

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

Cosmological observations in scalar-tensor quintessence (2001, methodology): “[55], we can give the perturbed Einstein equations”
The global non-linear stability of the Kerr-de Sitter family of black holes (2016, methodology): “For us, the most convenient formulation, which we use heavily in §7, is due to Ishibashi, Kodama and Seto [93], [92], [86], building on earlier work by Kodama–Sasaki [94].”
Generalized Uncertainty Principle: Approaches and Applications (2014, background): “For completeness, we mention that the perturbations typically give a much smaller contribution to the cosmic microwave background (CMB) radiation anisotropy than the inflationary adiabatic scalar perturbations [182].”
Inflation, Cosmic Perturbations and Non-Gaussianities (2013, background): “There have been already many books, reviews and lecture notes in this area [9–22].”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “20), the species which interact with quintessence are characterized by a mass function that changes in time [686, 45, 47, 947].”
Dark energy or modified gravity? An effective field theory approach (2012, methodology): “4On the other hand, nonlocal operators can arise starting from the local action (2.1) when one integrates out the non-dynamical metric variables (the lapse and shift) to obtain the analog of the Mukhanov-Sasaki action for just the remaining scalar degree of freedom.”
Occurrence of exact R2 inflation in non-local UV-complete gravity (2016, background): “We stress that the formula for the variation of the Weyl tensor presented in [78] does not provide a traceless tensor as it should.”
Modified Gravity and Cosmology (2011, methodology): “To study this we use the standard four-dimensional formalism [90, 717, 469, 917], decomposing the system into scalar, vector and tensor perturbations with respect to the spatial diffeomorphism group in the background cosmology.”
High-order Stochastic Simulation of Complex Spatially Distributed Natural Phenomena (2010, background): “High-order cumulants are combinations of moment statistical parameters that characterize nonGaussian random variables (Billinger and Rosenblatt 1966) and may be seen as an extension of the well-known covariance function.”
f(R) Theories (2010, background): “1 Perturbation equations We start with a general perturbed metric about the flat FLRW background [57, 352, 231, 232, 437]”
Correlation functions in stochastic inflation (2015, background): “One possible choice is the Mukhanov–Sasaki variable [7,41,94] v, which can be defined, order by order, as the scalar field fluctuation φ(n) on uniform curvature hypersurfaces [95].”
New physics from the polarized light of the cosmic microwave background (2022, background): “The so-called scalar-vector-tensor decomposition theorem states that scalar, vector, and tensor modes are decoupled and evolve independently of each other at first order in perturbation, when the background spacetime is homogeneous and isotropic 202 .”
Gauge fields and inflation (2012, background): “Non-Gaussianity may be defined in terms of the Bardeen potential Φ, Φ(x) = Φg(x) + f local NL (Φ 2 g(x)− 〈Φ(2)g(x)〉), which during the matter era and at the linear order is Φ = 35R [23].”
DE SITTER MUSINGS (2012, background): “Similarly, given that the global geometry is contracting if we begin at I−, a large class of data at I− will never (2)Though we do not discuss linearized gravity in a fixed de Sitter background in this article, a very complete discussion can be found in [14, 15].”