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...
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Physical Review D; Vol. 71, No. 12
2005
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| Acceso en línea: | http://babel.banrepcultural.org/cdm/ref/collection/p17054coll23/id/454 |
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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 |
12,131701 |