Brane Inflation: String Theory Viewed from the Cosmos

Tye, S.‐H. Henry

doi:10.1007/978-3-540-74233-3_28

Cited by 150 publications

(106 citation statements)

References 93 publications

(128 reference statements)

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“…(18) is constant. This inevitably introduces errors into the bound (27). However, the two limiting cases of interest in KS-type geometries arise when the warp factor scales either as h ∝ ρ or as h ≃ constant [39,40].…”

Section: An Upper Bound On the Primordial Gravitational Wavesmentioning

confidence: 99%

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Gravitational wave constraints on Dirac–Born–Infeld inflation

Lidsey¹,

Huston²

2007

J. Cosmol. Astropart. Phys.

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Abstract. An upper bound on the amplitude of the primordial gravitational wave spectrum generated during ultra-violet DBI inflation is derived. The bound is insensitive to the form of the inflaton potential and the warp factor of the compactified dimensions and can be expressed entirely in terms of observational parameters once the volume of the five-dimensional sub-manifold of the throat has been specified. For standard type IIB compactification schemes, the bound predicts undetectably small tensor perturbations with a tensor-scalar ratio r < 10 −7 . This is incompatible with a corresponding lower limit of r > 0.1(1 − n s ), which applies to any model that generates a red spectral index n s < 1 and a potentially detectable non-Gaussianity in the curvature perturbation. Possible ways of evading these bounds in more general DBItype scenarios are discussed and a multiple-brane model is investigated as a specific example.

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Section: An Upper Bound On the Primordial Gravitational Wavesmentioning

confidence: 99%

“…(For recent reviews, see, e.g., [27,28]). Of particular interest is the DBI inflationary scenario [7,12].…”

Section: Introductionmentioning

confidence: 99%

Gravitational wave constraints on Dirac–Born–Infeld inflation

Lidsey¹,

Huston²

2007

J. Cosmol. Astropart. Phys.

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“…The higher curvature terms may offer the alternative to the use of dynamical moduli, warped compactifications, or engineering desirable brane configurations [2,3,12], since all those popular mechanisms need many ad hoc assumptions about a non-perturbative off-shell effective action of M-theory, while no explanation is provided why certain brane configurations are to be considered and how they arise.…”

Section: Resultsmentioning

confidence: 99%

On the Quartic Curvature Gravity in the Context of FRW Cosmology

Iihoshi

Ketov

2008

Int. J. Mod. Phys. A

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We consider the purely gravitational fourth-order (in the spacetime curvature) quantum corrections to the Einstein-Hilbert gravity action, coming from superstrings in the leading order with respect to the Regge slope parameter, and study their impact on the evolution of the Hubble scale in the context of the FRW cosmology, in four spacetime dimensions. We propose the generalized Friedmann equations, and rule out the most naive (Bel-Robinson tensor squared) gravity. Our new cosmological equations have exact inflationary solutions without a spacetime singularity.

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“…It is therefore of both theoretical and observational interest to look for inflationary properties that are, or will be in a foreseeable future, significant enough in the data to allow disambiguation between the different models. Many works are devoted to this task ranging from the details of the reheating era to the search of a theoretical embedding of inflation in supersymmetry or string theory [2,3,4,5]. In the following, we will be interested in the model disambiguation problem through the cosmological perturbations and the Cosmic Microwave Background (CMB) anisotropies.…”

Section: Motivationsmentioning

confidence: 99%

The Numerical Treatment of Inflationary Models

Ringeval¹

Inflationary Cosmology

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Summary. The precision reached by the recent CMB measurements gives new insights into the shape of the primordial power spectra of the cosmological perturbations. In the context of inflationary cosmology, this implies that the CMB data are now sensitive to the form of the inflaton potential. Most of the current approaches devoted to the derivation of the inflationary primordial power spectra, or to the inflaton potential reconstruction problem, rely on approximate analytical treatments that may break down for exotic models. In this article, we numerically solve the inflationary evolution of both the background and all the perturbed quantities to extract the primordial power spectra exactly. Such a method solely relies on General Relativity and linear perturbation theory. More than providing a tool to test analytical approximations, one may consider, without complications, the treatment of non-standard inflationary models as those involving several fields, eventually nonminimally coupled to gravity.The usefulness of the exact numerical approach to deal with CMB data is illustrated by analysing the WMAP third year data in the context of single field models. For this purpose, we introduce a new inflationary related parameter encoding the basic properties of the reheating era. This reheating parameter has significant observable effects and provides a self-consistency test of inflationary models. As a working example, the marginalised probability distributions of the reheating and potential parameters associated with the small field models are presented.

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Brane Inflation: String Theory Viewed from the Cosmos

Cited by 150 publications

References 93 publications

Gravitational wave constraints on Dirac–Born–Infeld inflation

Gravitational wave constraints on Dirac–Born–Infeld inflation

On the Quartic Curvature Gravity in the Context of FRW Cosmology

The Numerical Treatment of Inflationary Models

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