Electromagnetic origin of the CMB anisotropy in string cosmology

In the inflationary scenarios suggested by string theory, the vacuum fluctuations of the electromagnetic field can be amplified by the time-evolution of the dilaton background, and can grow large enough to explain both the origin of the cosmic magnetic fields and of the observed CMB anisotropy. The...

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Detalles Bibliográficos
Autores principales: Gasperini, M., Giovannini, Massimo, Veneziano, G.
Lenguaje:eng
Publicado: 1995
Materias:
Astrophysics and Astronomy
Acceso en línea:https://dx.doi.org/10.1103/PhysRevD.52.R6651
http://cds.cern.ch/record/281511
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author Gasperini, M.
Giovannini, Massimo
Veneziano, G.
author_facet Gasperini, M.
Giovannini, Massimo
Veneziano, G.
author_sort Gasperini, M.
collection CERN
description In the inflationary scenarios suggested by string theory, the vacuum fluctuations of the electromagnetic field can be amplified by the time-evolution of the dilaton background, and can grow large enough to explain both the origin of the cosmic magnetic fields and of the observed CMB anisotropy. The normalization of the perturbation spectrum is fixed, and implies a relation between the perturbation amplitude at the COBE scale and the spectral index n. Working within a generic two-parameter family of backgrounds, a large scale anisotropy \Delta T/T\simeq 10^{-5} is found to correspond to a spectral index in the range n\simeq 1.11 - 1.17.
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institution Organización Europea para la Investigación Nuclear
language eng
publishDate 1995
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spelling cern-2815112023-03-14T17:14:23Zdoi:10.1103/PhysRevD.52.R6651http://cds.cern.ch/record/281511engGasperini, M.Giovannini, MassimoVeneziano, G.Electromagnetic origin of the CMB anisotropy in string cosmologyAstrophysics and AstronomyIn the inflationary scenarios suggested by string theory, the vacuum fluctuations of the electromagnetic field can be amplified by the time-evolution of the dilaton background, and can grow large enough to explain both the origin of the cosmic magnetic fields and of the observed CMB anisotropy. The normalization of the perturbation spectrum is fixed, and implies a relation between the perturbation amplitude at the COBE scale and the spectral index n. Working within a generic two-parameter family of backgrounds, a large scale anisotropy \Delta T/T\simeq 10^{-5} is found to correspond to a spectral index in the range n\simeq 1.11 - 1.17.In the inflationary scenarios suggested by string theory, the vacuum fluctuations of the electromagnetic field can be amplified by the time-evolution of the dilaton background, and can grow large enough to explain both the origin of the cosmic magnetic fields and of the observed CMB anisotropy. The normalization of the perturbation spectrum is fixed, and implies a relation between the perturbation amplitude at the COBE scale and the spectral index $n$. Working within a generic two-parameter family of backgrounds, a large scale anisotropy $\Delta T/T\simeq 10~{-5}$ is found to correspond to a spectral index in the range $n\simeq 1.11 - 1.17$.astro-ph/9505041CERN-TH-95-102DFTT-28-95CERN-TH-95-102DFTT-95-28oai:cds.cern.ch:2815111995-05-09
spellingShingle Astrophysics and Astronomy
Gasperini, M.
Giovannini, Massimo
Veneziano, G.
Electromagnetic origin of the CMB anisotropy in string cosmology
title Electromagnetic origin of the CMB anisotropy in string cosmology
title_full Electromagnetic origin of the CMB anisotropy in string cosmology
title_fullStr Electromagnetic origin of the CMB anisotropy in string cosmology
title_full_unstemmed Electromagnetic origin of the CMB anisotropy in string cosmology
title_short Electromagnetic origin of the CMB anisotropy in string cosmology
title_sort electromagnetic origin of the cmb anisotropy in string cosmology
topic Astrophysics and Astronomy
url https://dx.doi.org/10.1103/PhysRevD.52.R6651
http://cds.cern.ch/record/281511
work_keys_str_mv AT gasperinim electromagneticoriginofthecmbanisotropyinstringcosmology
AT giovanninimassimo electromagneticoriginofthecmbanisotropyinstringcosmology
AT venezianog electromagneticoriginofthecmbanisotropyinstringcosmology

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