Non-gaussianity from the second-order cosmological perturbation

Cosmological scales leave the horizon during in?ation and reenter it after big bang nucleosynthesis. Throughout the superhorizon era it is very useful to de?ne a primordial cosmological curvature perturbation, which is conserved if and only if pressure throughout the Universe is a unique function of...

Descripción completa

Detalles Bibliográficos
Autor Principal: Lyth, David H.; Rodríguez García, Yeinzon
Formato: Artículo (Article)
Lenguaje:Desconocido (Unknown)
Publicado: Physical Review D; Vol. 71, No. 12 2005
Materias:
Acceso en línea:http://babel.banrepcultural.org/cdm/ref/collection/p17054coll23/id/454
id ir-p17054coll23-454
recordtype dspace
spelling ir-p17054coll23-4542020-09-28 Non-gaussianity from the second-order cosmological perturbation Lyth, David H.; Rodríguez García, Yeinzon Cosmological scales leave the horizon during in?ation and reenter it after big bang nucleosynthesis. Throughout the superhorizon era it is very useful to de?ne a primordial cosmological curvature perturbation, which is conserved if and only if pressure throughout the Universe is a unique function of energy density (the adiabatic pressure condition) [1–7]. Observation directly constrains the curvature perturbation at the very end of the superhorizon era, a few Hubble times before cosmological scales start to enter the horizon, when it apparently sets the initial condition for the subsequent evolution of all cosmological perturbations. The observed curvature perturbation is almost Gaussian with an almost scale-invariant spectrum. Cosmología; Física; Teorema de Gauss Ciencias naturales y matemáticas; Ciencias naturales y matemáticas / Física 2005 Physical Review D; Vol. 71, No. 12 PDF Artículo ENG - Inglés Colfuturo © Derechos reservados del autor http://babel.banrepcultural.org/cdm/ref/collection/p17054coll23/id/454
institution Biblioteca Virtual Banco de la República - Colecciones digitales
collection Custom
language Desconocido (Unknown)
topic Cosmología; Física; Teorema de Gauss
Ciencias naturales y matemáticas; Ciencias naturales y matemáticas / Física
spellingShingle Cosmología; Física; Teorema de Gauss
Ciencias naturales y matemáticas; Ciencias naturales y matemáticas / Física
Lyth, David H.; Rodríguez García, Yeinzon
Non-gaussianity from the second-order cosmological perturbation
description Cosmological scales leave the horizon during in?ation and reenter it after big bang nucleosynthesis. Throughout the superhorizon era it is very useful to de?ne a primordial cosmological curvature perturbation, which is conserved if and only if pressure throughout the Universe is a unique function of energy density (the adiabatic pressure condition) [1–7]. Observation directly constrains the curvature perturbation at the very end of the superhorizon era, a few Hubble times before cosmological scales start to enter the horizon, when it apparently sets the initial condition for the subsequent evolution of all cosmological perturbations. The observed curvature perturbation is almost Gaussian with an almost scale-invariant spectrum.
format Artículo (Article)
author Lyth, David H.; Rodríguez García, Yeinzon
author_facet Lyth, David H.; Rodríguez García, Yeinzon
author_sort Lyth, David H.; Rodríguez García, Yeinzon
title Non-gaussianity from the second-order cosmological perturbation
title_short Non-gaussianity from the second-order cosmological perturbation
title_full Non-gaussianity from the second-order cosmological perturbation
title_fullStr Non-gaussianity from the second-order cosmological perturbation
title_full_unstemmed Non-gaussianity from the second-order cosmological perturbation
title_sort non-gaussianity from the second-order cosmological perturbation
publisher Physical Review D; Vol. 71, No. 12
publishDate 2005
url http://babel.banrepcultural.org/cdm/ref/collection/p17054coll23/id/454
_version_ 1682459954944933888
score 11,489418