Cosmological Inflation and Large-Scale Structure

By R. Daly. 2001

1,762 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/242fc7934e4d171381cbe9d088c9cc7478b501d3

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Citations in the corpus

LRS Bianchi type I models with anisotropic dark energy and constant deceleration parameter (2008, neutral): “48 67 v2 [ gr -q c] 1”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “The deviation from scale-invariance of the scalar spectrum is characterized by the spectral index ns, defined by (see, for instance, [570])”
Inflation from warped space (2005, background): “This time delay seeds the large scale structure formation [6,7,56,57].”
Power-spectrum normalization from the local abundance of rich clusters of galaxies (2001, background): “The spherical top-hat ansatz (Peebles 1993; Liddle & Lyth 2000; Peacock 1999) models the formation of an object by the evolution of a spherical overdense region embedded in a homogeneous ‘background’ of mean density ρ̄.”
The emergent universe: an explicit construction (2003, background): “The duration of the slow-rolling inflationary regime, in a spatially flat model, is determined by the usual slow-roll parameters [17] (φ) = 1 2 M(2) Pl ( V ′”
Gravitino production by primordial black hole evaporation and constraints on the inhomogeneity of the early universe (2004, background): “In the standard cosmological paradigm of inflation, the primordial power spectrum is expected to be nearly—but not exactly—scale invariant [41].”
Inflation models and observation (2005, background): “1 Standard results about early-universe cosmology and observation are described for instance in [1, 2].”
Axion cosmology and the energy scale of inflation (2008, background): “A multitude of inflation models involving a broad range of energy scales have been discussed in the literature, including chaotic inflation [4], brane inflation [5, 6] and others [7].”
Detecting a small perturbation through its non-Gaussianity (2005, background): “The origin of structure in the Universe seems to be the primordial curvature perturbation ζ, present already a few Hubble times before cosmological scales enter the horizon and come into causal contact [1].”
Quantum diffusion during inflation and primordial black holes (2017, background): “In order to use the slow-roll approximation, one needs to check that the slow-roll conditions [90], M2 Pl(v ′/v)2 1, M2 Pl|v/v| 1, and M4 Pl|vv/v(2)| 1, are satisfied.”
Cosmology with inhomogeneous magnetic fields (2006, background): “For example, isocurvature initial conditions typically correspond to zero perturbation in the total energy density [163,165].”
Random matrices and the spectrum of N-flation (2005, background): “The controllability of these models is a subject of debate [8], and depends strongly on the relation between particle physics and gravity near the Planck scale.”
Cosmology and brane worlds: a review (2003, neutral): “The amplitude of scalar perturbations is [50] A(2)S = 4〈ζ2〉/25.”
Inflationary paradigm in trouble after Planck2013 (2013, methodology): “– initial smoothness on the scale of a billion or more Hubble volumes [25]! In sum, by favoring only plateau-like models, the Planck2013 data creates a serious new challenge for the inflationary paradigm: the universally accepted assumption about initial conditions no longer leads to inflation; inst”
Possible signals of vacuum dynamics in the Universe (2017, background): “…VACUUM Despite the theory of cosmological perturbations has been discussed at length in several specialized textbooks, see e.g. (Peebles 1993; Liddle & Lyth 2000, 2009; Dodelson 2003), the dynamical character of the vacuum produces some changes on the standard equations which are worth…”
The primordial curvature perturbation in the ekpyrotic universe. (2001, background): “(13) The curvature perturbation generated during inflation Let us first summarize the way in which the vacuum fluctuation of the inflaton field φ generates the curvature perturbation [8, 9, 10].”
Cosmic clocks, cosmic variance and cosmic averages (2007, background): “Density perturbations at last scattering will, of course, give rise to temperature fluctuations in the CMBR through the dominant Sachs–Wolfe effect, and what I have just defined as the particle horizon volume selection bias is the reason for cosmic variance in the two-point angular correlation funct”
A general proof of the conservation of the curvature perturbation (2004, methodology): “Locally, this statement follows from the equations of the coordinate-free approach as given for instance in [39] and reviewed in [40](10).”