Impact of dark energy perturbations on the growth index
Autor(a) principal: | |
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Data de Publicação: | 2014 |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRN |
Texto Completo: | https://repositorio.ufrn.br/handle/123456789/30833 |
Resumo: | We show that in clustering dark energy models the growth index of linear matter perturbations, γ, can be much lower than in Λ CDM or smooth quintessence models and presents a strong variation with redshift. We find that the impact of dark energy perturbations on γ is enhanced if the dark energy equation of state has a large and rapid decay at low redshift. We study four different models with these features and show that we may have 0.33 < γ ( z ) < 0.48 at 0 < z < 3. We also show that the constant γ parametrization for the growth rate, f = d ln δ m / d lna = Ω γ m, is a few percent inaccurate for such models and that a redshift-dependent parametrization for γ can provide about four times more accurate fits for f. We discuss the robustness of the growth index to distinguish between general relativity with clustering dark energy and modified gravity models, finding that some f ( R ) and clustering dark energy models can present similar values for γ |
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Batista, Ronaldo Carlotto2020-12-04T20:19:52Z2020-12-04T20:19:52Z2014-06-13BATISTA, Ronaldo C.. Impact of dark energy perturbations on the growth index. Physical Review D, [S.L.], v. 89, n. 12, p. 123508-123508, 13 jun. 2014. Disponível em: https://journals.aps.org/prd/abstract/10.1103/PhysRevD.89.123508. Acesso em: 02 out. 2020. http://dx.doi.org/10.1103/physrevd.89.123508.1550-79981550-2368https://repositorio.ufrn.br/handle/123456789/3083310.1103/PhysRevD.89.123508American Physical SocietyDark energy equationImpact of dark energy perturbations on the growth indexinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articleWe show that in clustering dark energy models the growth index of linear matter perturbations, γ, can be much lower than in Λ CDM or smooth quintessence models and presents a strong variation with redshift. We find that the impact of dark energy perturbations on γ is enhanced if the dark energy equation of state has a large and rapid decay at low redshift. We study four different models with these features and show that we may have 0.33 < γ ( z ) < 0.48 at 0 < z < 3. We also show that the constant γ parametrization for the growth rate, f = d ln δ m / d lna = Ω γ m, is a few percent inaccurate for such models and that a redshift-dependent parametrization for γ can provide about four times more accurate fits for f. We discuss the robustness of the growth index to distinguish between general relativity with clustering dark energy and modified gravity models, finding that some f ( R ) and clustering dark energy models can present similar values for γengreponame:Repositório Institucional da UFRNinstname:Universidade Federal do Rio Grande do Norte (UFRN)instacron:UFRNinfo:eu-repo/semantics/openAccessLICENSElicense.txtlicense.txttext/plain; charset=utf-81484https://repositorio.ufrn.br/bitstream/123456789/30833/2/license.txte9597aa2854d128fd968be5edc8a28d9MD52ORIGINALImpactOfDarkEnergy_2014.pdfImpactOfDarkEnergy_2014.pdfapplication/pdf418156https://repositorio.ufrn.br/bitstream/123456789/30833/1/ImpactOfDarkEnergy_2014.pdfb23c62435414113fc0eb50a1698597f5MD51TEXTImpactOfDarkEnergy_2014.pdf.txtImpactOfDarkEnergy_2014.pdf.txtExtracted texttext/plain27833https://repositorio.ufrn.br/bitstream/123456789/30833/3/ImpactOfDarkEnergy_2014.pdf.txt0dabd04a0c5a76d10ffdfc2658da7341MD53THUMBNAILImpactOfDarkEnergy_2014.pdf.jpgImpactOfDarkEnergy_2014.pdf.jpgGenerated Thumbnailimage/jpeg1713https://repositorio.ufrn.br/bitstream/123456789/30833/4/ImpactOfDarkEnergy_2014.pdf.jpgf9f481a288b4b881d79f10e924218c4bMD54123456789/308332020-12-06 05:06:43.86oai:https://repositorio.ufrn.br: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Repositório de PublicaçõesPUBhttp://repositorio.ufrn.br/oai/opendoar:2020-12-06T08:06:43Repositório Institucional da UFRN - Universidade Federal do Rio Grande do Norte (UFRN)false |
dc.title.pt_BR.fl_str_mv |
Impact of dark energy perturbations on the growth index |
title |
Impact of dark energy perturbations on the growth index |
spellingShingle |
Impact of dark energy perturbations on the growth index Batista, Ronaldo Carlotto Dark energy equation |
title_short |
Impact of dark energy perturbations on the growth index |
title_full |
Impact of dark energy perturbations on the growth index |
title_fullStr |
Impact of dark energy perturbations on the growth index |
title_full_unstemmed |
Impact of dark energy perturbations on the growth index |
title_sort |
Impact of dark energy perturbations on the growth index |
author |
Batista, Ronaldo Carlotto |
author_facet |
Batista, Ronaldo Carlotto |
author_role |
author |
dc.contributor.author.fl_str_mv |
Batista, Ronaldo Carlotto |
dc.subject.por.fl_str_mv |
Dark energy equation |
topic |
Dark energy equation |
description |
We show that in clustering dark energy models the growth index of linear matter perturbations, γ, can be much lower than in Λ CDM or smooth quintessence models and presents a strong variation with redshift. We find that the impact of dark energy perturbations on γ is enhanced if the dark energy equation of state has a large and rapid decay at low redshift. We study four different models with these features and show that we may have 0.33 < γ ( z ) < 0.48 at 0 < z < 3. We also show that the constant γ parametrization for the growth rate, f = d ln δ m / d lna = Ω γ m, is a few percent inaccurate for such models and that a redshift-dependent parametrization for γ can provide about four times more accurate fits for f. We discuss the robustness of the growth index to distinguish between general relativity with clustering dark energy and modified gravity models, finding that some f ( R ) and clustering dark energy models can present similar values for γ |
publishDate |
2014 |
dc.date.issued.fl_str_mv |
2014-06-13 |
dc.date.accessioned.fl_str_mv |
2020-12-04T20:19:52Z |
dc.date.available.fl_str_mv |
2020-12-04T20:19:52Z |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/article |
format |
article |
status_str |
publishedVersion |
dc.identifier.citation.fl_str_mv |
BATISTA, Ronaldo C.. Impact of dark energy perturbations on the growth index. Physical Review D, [S.L.], v. 89, n. 12, p. 123508-123508, 13 jun. 2014. Disponível em: https://journals.aps.org/prd/abstract/10.1103/PhysRevD.89.123508. Acesso em: 02 out. 2020. http://dx.doi.org/10.1103/physrevd.89.123508. |
dc.identifier.uri.fl_str_mv |
https://repositorio.ufrn.br/handle/123456789/30833 |
dc.identifier.issn.none.fl_str_mv |
1550-7998 1550-2368 |
dc.identifier.doi.none.fl_str_mv |
10.1103/PhysRevD.89.123508 |
identifier_str_mv |
BATISTA, Ronaldo C.. Impact of dark energy perturbations on the growth index. Physical Review D, [S.L.], v. 89, n. 12, p. 123508-123508, 13 jun. 2014. Disponível em: https://journals.aps.org/prd/abstract/10.1103/PhysRevD.89.123508. Acesso em: 02 out. 2020. http://dx.doi.org/10.1103/physrevd.89.123508. 1550-7998 1550-2368 10.1103/PhysRevD.89.123508 |
url |
https://repositorio.ufrn.br/handle/123456789/30833 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.publisher.none.fl_str_mv |
American Physical Society |
publisher.none.fl_str_mv |
American Physical Society |
dc.source.none.fl_str_mv |
reponame:Repositório Institucional da UFRN instname:Universidade Federal do Rio Grande do Norte (UFRN) instacron:UFRN |
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Universidade Federal do Rio Grande do Norte (UFRN) |
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UFRN |
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