Home > Research > Publications & Outputs > Trapped Quintessential Inflation from Flux Comp...
View graph of relations

Trapped Quintessential Inflation from Flux Compactifications.

Research output: Contribution in Book/Report/Proceedings - With ISBN/ISSNChapter

Published

Standard

Trapped Quintessential Inflation from Flux Compactifications. / Dimopoulos, Konstantinos.

IDM 2006: 6th International Workshop On The Identification Of Dark Matter. ed. / M. Axenides; G. Fanourakis; J. Vergados. World Scientific, 2007. p. 635-646.

Research output: Contribution in Book/Report/Proceedings - With ISBN/ISSNChapter

Harvard

Dimopoulos, K 2007, Trapped Quintessential Inflation from Flux Compactifications. in M Axenides, G Fanourakis & J Vergados (eds), IDM 2006: 6th International Workshop On The Identification Of Dark Matter. World Scientific, pp. 635-646.

APA

Dimopoulos, K. (2007). Trapped Quintessential Inflation from Flux Compactifications. In M. Axenides, G. Fanourakis, & J. Vergados (Eds.), IDM 2006: 6th International Workshop On The Identification Of Dark Matter (pp. 635-646). World Scientific.

Vancouver

Dimopoulos K. Trapped Quintessential Inflation from Flux Compactifications. In Axenides M, Fanourakis G, Vergados J, editors, IDM 2006: 6th International Workshop On The Identification Of Dark Matter. World Scientific. 2007. p. 635-646

Author

Dimopoulos, Konstantinos. / Trapped Quintessential Inflation from Flux Compactifications. IDM 2006: 6th International Workshop On The Identification Of Dark Matter. editor / M. Axenides ; G. Fanourakis ; J. Vergados. World Scientific, 2007. pp. 635-646

Bibtex

@inbook{762672bb1e504903a76c43ba105e97a9,
title = "Trapped Quintessential Inflation from Flux Compactifications.",
abstract = "It is investigated whether a massive Abelian vector field, whose gauge kinetic function is growing during inflation, can be responsible for the generation of the curvature perturbation in the Universe. Particle production is studied and it is shown that the vector field can obtain a scale invariant superhorizon spectrum of perturbations with a reasonable choice of kinetic function. After inflation the vector field begins coherent oscillations, during which it corresponds to pressureless isotropic matter. When the vector field dominates the Universe its perturbations give rise to the observed curvature perturbation following the curvaton scenario. It is found that this is possible if, after the end of inflation, the mass of the vector field increases at a phase transition at temperature of order 1 TeV or lower. Inhomogeneous reheating, whereby the vector field modulates the decay rate of the inflaton, is also studied.",
author = "Konstantinos Dimopoulos",
year = "2007",
language = "English",
pages = "635--646",
editor = "M. Axenides and G. Fanourakis and J. Vergados",
booktitle = "IDM 2006: 6th International Workshop On The Identification Of Dark Matter",
publisher = "World Scientific",

}

RIS

TY - CHAP

T1 - Trapped Quintessential Inflation from Flux Compactifications.

AU - Dimopoulos, Konstantinos

PY - 2007

Y1 - 2007

N2 - It is investigated whether a massive Abelian vector field, whose gauge kinetic function is growing during inflation, can be responsible for the generation of the curvature perturbation in the Universe. Particle production is studied and it is shown that the vector field can obtain a scale invariant superhorizon spectrum of perturbations with a reasonable choice of kinetic function. After inflation the vector field begins coherent oscillations, during which it corresponds to pressureless isotropic matter. When the vector field dominates the Universe its perturbations give rise to the observed curvature perturbation following the curvaton scenario. It is found that this is possible if, after the end of inflation, the mass of the vector field increases at a phase transition at temperature of order 1 TeV or lower. Inhomogeneous reheating, whereby the vector field modulates the decay rate of the inflaton, is also studied.

AB - It is investigated whether a massive Abelian vector field, whose gauge kinetic function is growing during inflation, can be responsible for the generation of the curvature perturbation in the Universe. Particle production is studied and it is shown that the vector field can obtain a scale invariant superhorizon spectrum of perturbations with a reasonable choice of kinetic function. After inflation the vector field begins coherent oscillations, during which it corresponds to pressureless isotropic matter. When the vector field dominates the Universe its perturbations give rise to the observed curvature perturbation following the curvaton scenario. It is found that this is possible if, after the end of inflation, the mass of the vector field increases at a phase transition at temperature of order 1 TeV or lower. Inhomogeneous reheating, whereby the vector field modulates the decay rate of the inflaton, is also studied.

M3 - Chapter

SP - 635

EP - 646

BT - IDM 2006: 6th International Workshop On The Identification Of Dark Matter

A2 - Axenides, M.

A2 - Fanourakis, G.

A2 - Vergados, J.

PB - World Scientific

ER -