Chaotic inflation as an attractor in initial-condition space

Kung, J. H.; Brandenberger, Robert H.

doi:10.1103/physrevd.42.1008

Cited by 80 publications

(64 citation statements)

References 41 publications

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“…Furthermore, the initially large gradient terms also can in turn induce large kinetic energy in the modes. The outcome found in [7,11,13] (see also [9]) for this case is that the universe expansion is noninflationary. On the other hand, for the excited k/a > H modes with smaller amplitudes, their evolution will be oscillatory and once again the universe expansion is noninflationary.…”

Section: A Scalar Fieldmentioning

confidence: 69%

“…For supercooled inflation, the effect of such interactions has been considered from the perspective of mode mixing for some special cases in [8,9] and through computer simulations of scalar fields in one spatial dimension in [10,11]. Up to the scope of these works, their analysis concludes that nonlinear interactions do not present any additional complications to the initial condition problem.…”

Section: A Scalar Fieldmentioning

confidence: 99%

“…For scalar field driven inflation, the general dynamical conditions necessary for a finite spatial patch to initiate and sustain inflation have been considered in [7][8][9][10][11][12] and a comprehensive review has been given in [13]. Here the requirements addressed in these works, primarily the review [13], will be systematically examined with emphasis on determining their implications for the minimal initial inflationary patch size.…”

Section: A Scalar Fieldmentioning

confidence: 99%

“…By embedding we mean matching the inflationary space time with the background space time at the boundary of the patch. Second, it must be shown that for t > t i , the patch is dynamically stable to sustain inflation [7][8][9][10][11][12][13]. For example, large fluctuations, which conceivably could enter the inflating patch at a maximum rate limited only by causality, should not destroy the inflationary conditions within the patch.…”

Section: Introductionmentioning

confidence: 99%

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Inflationary initial conditions consistent with causality

Berera

Gordon

2001

Phys. Rev. D

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The initial condition problem of inflation is examined from the perspective of both spacetime embedding and scalar field dynamics. The spacetime embedding problem is solved for arbitrary initial spatial curvature Ω, which generalizes previous works that primarily treat the flat case Ω = 1. Scalar field dynamics that is consistent with the embedding constraints are examined, with the additional treatment of damping effects. The effects of inhomogeneities on the embedding problem also are considered. A category of initial conditions are identified that are not acausal and can develop into an inflationary regime.

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Section: A Scalar Fieldmentioning

confidence: 69%

Section: A Scalar Fieldmentioning

confidence: 99%

Section: A Scalar Fieldmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Inflationary initial conditions consistent with causality

Berera

Gordon

2001

Phys. Rev. D

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“…Consequently, the scalar field would require much more than the available time to relax to thermal equilibrium. This difficulty may not be crucial, however, because true thermal equilibrium is not really necessary: a variety of random configurations give results that are very similar to those of thermal equilibrium (9)(10)(11)(12).…”

Section: The Inflationary Universe Scenariomentioning

confidence: 99%

Inflation.

Guth

1993

Proc. Natl. Acad. Sci. U.S.A.

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A short review of inflation is given, starting with a description of the underlying mechanism and the scenario of events. Four variations-old inflation, new inflation, chaotic inflation, and extended inflation-are discussed. It is claimed that the inflationary model provides a plausible explanation for (i) the large number of particles in the universe,(ii) the Hubble expansion, (iii) the large-scale uniformity of the universe, (iv) the nearness of the universe to a critical density, (v) the absence of magnetic monopoles, and (vi) the scaleinvariant spectrum of microwave background fluctuations observed by COBE (Cosmic Background Explorer). Finally, it is argued that the plausibility ofinflation is enhanced by the fact that inflation is eternal.The inflationary model is a modification of the standard big bang model that provides answers to a number of questions that the standard model fails to address. The inflationary period lasts for only a small fraction of a second, and then the inflationary model joins smoothly onto the standard model. The role of inflation is to set up the initial conditions for the standard model, conditions which otherwise would have to be assumed without explanation. Before inflation the total mass contained in the universe could have been as small as 10 kg. If inflation is right, then the inflationary mechanism is responsible for producing essentially all of the matter, energy, and entropy that exists in the universe today.In this lecture I will give a brief review of inflation, describing the mechanism of inflation, the outline of the scenario, the different types of inflationary models, and the evidence for inflation. Finally I will briefly discuss the eternal nature of inflation: once inflation begins, calculations indicate that it ends locally but not globally. Although this property does not appear to lead to any observable predictions, it certainly affects the way we think about the universe as a whole. I. The Mechanism of InflationBefore explaining the arguments for inflation, I will first explain how the inflationary model works.The mechanism of inflation depends on scalar fields, so I will begin by briefly summarizing the role of scalar fields in particle physics. To begin with, the reader should recognize that in the context of modern particle physics, all fundamental particles are described by fields. The best known example is the photon. The classical equations describing the electromagnetic field were written down in the 1860s, but then in the early 20th century physicists learned that the underlying laws of nature are quantum and not classical. The quantization of the electromagnetic field can be carried out in a very straightforward way. For simplicity one can consider the fields insideThe publication costs of this article were defrayed in part by page charge payment. This article must therefore be hereby marked "advertisement" in accordance with 18 U.S.C. §1734 solely to indicate this fact. a box, letting the size of the box approach infinity at the end of the c...

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Theory of Cosmological Perturbations and Applications to Superstring Cosmology

Brandenberger

2005

String Theory: From Gauge Interactions to Cosmology

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The theory of cosmological perturbations is the main tool which connects theories of the early Universe (based on new fundamental physics such as string theory) with cosmological observations. In these lectures, I will provide an introduction to this theory, beginning with an overview of the Newtonian theory of fluctuations, moving on to the analysis of fluctuations in the realm of classical general relativity, and culminating with a discussion of the quantum theory of cosmological perturbations. I will illustrate the formalism with applications to inflationary cosmology. I will review the basics of inflationary cosmology and discuss why -through the evolution of fluctuations -inflation may provide a way of observationally testing Planck-scale physics.

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Chaotic inflation as an attractor in initial-condition space

Cited by 80 publications

References 41 publications

Inflationary initial conditions consistent with causality

Inflationary initial conditions consistent with causality

Inflation.

Theory of Cosmological Perturbations and Applications to Superstring Cosmology

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