Time variation of the fine structure constant in the early universe and the Bekenstein model

Aims.We calculate the bounds on the variation in the fine structure constant at the time of primordial nucleosynthesis and at the time of neutral hydrogen formation. We used these bounds and other bounds from the late universe to test the Bekenstein model. Methods.We modified the Kawano code, CAMB,...

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Autores: Mosquera, Mercedes Elisa, Scóccola, Claudia Graciela, Landau, Susana Judith, Vucetich, Héctor
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2008
País:Argentina
Institución:Universidad Nacional de La Plata
Repositorio:SEDICI (UNLP)
Idioma:inglés
OAI Identifier:oai:sedici.unlp.edu.ar:10915/83101
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/83101
Access Level:acceso abierto
Palabra clave:Ciencias Astronómicas
Cosmic microwave background
Cosmology: theory
Early Universe
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spelling Time variation of the fine structure constant in the early universe and the Bekenstein modelMosquera, Mercedes ElisaScóccola, Claudia GracielaLandau, Susana JudithVucetich, HéctorCiencias AstronómicasCosmic microwave backgroundCosmology: theoryEarly UniverseAims.We calculate the bounds on the variation in the fine structure constant at the time of primordial nucleosynthesis and at the time of neutral hydrogen formation. We used these bounds and other bounds from the late universe to test the Bekenstein model. Methods.We modified the Kawano code, CAMB, and CosmoMC to include the possible variation in the fine structure constant. We used observational primordial abundances of D, <SUP>4</SUP>He, and <SUP>7</SUP>Li, recent data from the cosmic microwave background, and the 2dFGRS power spectrum, to obtain bounds on the variation in α. We calculated a piecewise solution to the scalar field equation of the Bekenstein model in two different regimes: i) matter and radiation, ii) matter and cosmological constant. We match both solutions with the appropriate boundary conditions. We performed a statistical analysis, using the bounds obtained from the early universe and other bounds from the late universe to constrain the free parameters of the model. Results.Results are consistent with no variation in α for the early universe. Limits on α are inconsistent with the scale length of the theory being larger than the Planck scale.Conclusions.In order to fit all observational and experimental data, the assumption l>L<SUB>p</SUB> implied in Bekenstein's model has to be relaxed.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2008info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf675-684http://sedici.unlp.edu.ar/handle/10915/83101enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20078605info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2024-05-08T12:53:43Zoai:sedici.unlp.edu.ar:10915/83101Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292024-05-08 12:53:44.077SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Time variation of the fine structure constant in the early universe and the Bekenstein model
title Time variation of the fine structure constant in the early universe and the Bekenstein model
spellingShingle Time variation of the fine structure constant in the early universe and the Bekenstein model
Mosquera, Mercedes Elisa
Ciencias Astronómicas
Cosmic microwave background
Cosmology: theory
Early Universe
title_short Time variation of the fine structure constant in the early universe and the Bekenstein model
title_full Time variation of the fine structure constant in the early universe and the Bekenstein model
title_fullStr Time variation of the fine structure constant in the early universe and the Bekenstein model
title_full_unstemmed Time variation of the fine structure constant in the early universe and the Bekenstein model
title_sort Time variation of the fine structure constant in the early universe and the Bekenstein model
dc.creator.none.fl_str_mv Mosquera, Mercedes Elisa
Scóccola, Claudia Graciela
Landau, Susana Judith
Vucetich, Héctor
author Mosquera, Mercedes Elisa
author_facet Mosquera, Mercedes Elisa
Scóccola, Claudia Graciela
Landau, Susana Judith
Vucetich, Héctor
author_role author
author2 Scóccola, Claudia Graciela
Landau, Susana Judith
Vucetich, Héctor
author2_role author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Cosmic microwave background
Cosmology: theory
Early Universe
topic Ciencias Astronómicas
Cosmic microwave background
Cosmology: theory
Early Universe
description Aims.We calculate the bounds on the variation in the fine structure constant at the time of primordial nucleosynthesis and at the time of neutral hydrogen formation. We used these bounds and other bounds from the late universe to test the Bekenstein model. Methods.We modified the Kawano code, CAMB, and CosmoMC to include the possible variation in the fine structure constant. We used observational primordial abundances of D, <SUP>4</SUP>He, and <SUP>7</SUP>Li, recent data from the cosmic microwave background, and the 2dFGRS power spectrum, to obtain bounds on the variation in α. We calculated a piecewise solution to the scalar field equation of the Bekenstein model in two different regimes: i) matter and radiation, ii) matter and cosmological constant. We match both solutions with the appropriate boundary conditions. We performed a statistical analysis, using the bounds obtained from the early universe and other bounds from the late universe to constrain the free parameters of the model. Results.Results are consistent with no variation in α for the early universe. Limits on α are inconsistent with the scale length of the theory being larger than the Planck scale.Conclusions.In order to fit all observational and experimental data, the assumption l>L<SUB>p</SUB> implied in Bekenstein's model has to be relaxed.
publishDate 2008
dc.date.none.fl_str_mv 2008
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/83101
url http://sedici.unlp.edu.ar/handle/10915/83101
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-6361
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20078605
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
675-684
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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