Can dark matter–dark energy interaction alleviate the cosmic coincidence problem?
Autor(a) principal: | |
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Data de Publicação: | 2022 |
Outros Autores: | , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1140/epjc/s10052-022-10234-y http://hdl.handle.net/11449/230664 |
Resumo: | In this paper we study a model of interacting dark energy–dark matter where the ratio between these components is not constant, changing from early to late times in such a way that the model can solve or alleviate the cosmic coincidence problem (CP). The interaction arises from an assumed relation of the form ρx∝ρdα, where ρx and ρd are the energy densities of dark energy and dark matter components, respectively, and α is a free parameter. For a dark energy equation of state parameter w= - 1 we found that, if α= 0 , the standard Λ CDM model is recovered, where the coincidence problem is unsolved. For 0 < α< 1 , the CP would be alleviated and for α∼ 1 , the CP would be solved. The dark energy component is analyzed with both w= - 1 and w≠ - 1. Using Supernovae type Ia and Hubble parameter data constraints, in the case w= - 1 we find α=0.109-0.072+0.062 at 68% C.L., and the CP is alleviated. For w≠ - 1 , a degeneracy arises on the w–α plane. In order to break such degeneracy we add cosmic microwave background distance priors and baryonic acoustic oscillations data to the constraints, yielding α= - 0.075 ± 0.046 at 68% C.L. In this case we find that the CP is not alleviated even for 2σ interval for α. Furthermore, this last model is discarded against flat Λ CDM according to BIC analysis. |
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Repositório Institucional da UNESP |
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spelling |
Can dark matter–dark energy interaction alleviate the cosmic coincidence problem?In this paper we study a model of interacting dark energy–dark matter where the ratio between these components is not constant, changing from early to late times in such a way that the model can solve or alleviate the cosmic coincidence problem (CP). The interaction arises from an assumed relation of the form ρx∝ρdα, where ρx and ρd are the energy densities of dark energy and dark matter components, respectively, and α is a free parameter. For a dark energy equation of state parameter w= - 1 we found that, if α= 0 , the standard Λ CDM model is recovered, where the coincidence problem is unsolved. For 0 < α< 1 , the CP would be alleviated and for α∼ 1 , the CP would be solved. The dark energy component is analyzed with both w= - 1 and w≠ - 1. Using Supernovae type Ia and Hubble parameter data constraints, in the case w= - 1 we find α=0.109-0.072+0.062 at 68% C.L., and the CP is alleviated. For w≠ - 1 , a degeneracy arises on the w–α plane. In order to break such degeneracy we add cosmic microwave background distance priors and baryonic acoustic oscillations data to the constraints, yielding α= - 0.075 ± 0.046 at 68% C.L. In this case we find that the CP is not alleviated even for 2σ interval for α. Furthermore, this last model is discarded against flat Λ CDM according to BIC analysis.Instituto de Ciências e Engenharia Universidade Estadual Paulista (UNESP), R. Geraldo Alckmin 519, SPDepartamento de Física Faculdade de Engenharia de Guaratinguetá Universidade Estadual Paulista (UNESP), Av. Dr. Ariberto Pereira da Cunha 333, SPInstituto de Ciências e Engenharia Universidade Estadual Paulista (UNESP), R. Geraldo Alckmin 519, SPDepartamento de Física Faculdade de Engenharia de Guaratinguetá Universidade Estadual Paulista (UNESP), Av. Dr. Ariberto Pereira da Cunha 333, SPUniversidade Estadual Paulista (UNESP)Jesus, J. F. [UNESP]Escobal, A. A. [UNESP]Benndorf, D. [UNESP]Pereira, S. H. [UNESP]2022-04-29T08:41:25Z2022-04-29T08:41:25Z2022-03-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttp://dx.doi.org/10.1140/epjc/s10052-022-10234-yEuropean Physical Journal C, v. 82, n. 3, 2022.1434-60521434-6044http://hdl.handle.net/11449/23066410.1140/epjc/s10052-022-10234-y2-s2.0-85127416496Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengEuropean Physical Journal Cinfo:eu-repo/semantics/openAccess2024-07-01T20:52:17Zoai:repositorio.unesp.br:11449/230664Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T18:02:14.688444Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
Can dark matter–dark energy interaction alleviate the cosmic coincidence problem? |
title |
Can dark matter–dark energy interaction alleviate the cosmic coincidence problem? |
spellingShingle |
Can dark matter–dark energy interaction alleviate the cosmic coincidence problem? Jesus, J. F. [UNESP] |
title_short |
Can dark matter–dark energy interaction alleviate the cosmic coincidence problem? |
title_full |
Can dark matter–dark energy interaction alleviate the cosmic coincidence problem? |
title_fullStr |
Can dark matter–dark energy interaction alleviate the cosmic coincidence problem? |
title_full_unstemmed |
Can dark matter–dark energy interaction alleviate the cosmic coincidence problem? |
title_sort |
Can dark matter–dark energy interaction alleviate the cosmic coincidence problem? |
author |
Jesus, J. F. [UNESP] |
author_facet |
Jesus, J. F. [UNESP] Escobal, A. A. [UNESP] Benndorf, D. [UNESP] Pereira, S. H. [UNESP] |
author_role |
author |
author2 |
Escobal, A. A. [UNESP] Benndorf, D. [UNESP] Pereira, S. H. [UNESP] |
author2_role |
author author author |
dc.contributor.none.fl_str_mv |
Universidade Estadual Paulista (UNESP) |
dc.contributor.author.fl_str_mv |
Jesus, J. F. [UNESP] Escobal, A. A. [UNESP] Benndorf, D. [UNESP] Pereira, S. H. [UNESP] |
description |
In this paper we study a model of interacting dark energy–dark matter where the ratio between these components is not constant, changing from early to late times in such a way that the model can solve or alleviate the cosmic coincidence problem (CP). The interaction arises from an assumed relation of the form ρx∝ρdα, where ρx and ρd are the energy densities of dark energy and dark matter components, respectively, and α is a free parameter. For a dark energy equation of state parameter w= - 1 we found that, if α= 0 , the standard Λ CDM model is recovered, where the coincidence problem is unsolved. For 0 < α< 1 , the CP would be alleviated and for α∼ 1 , the CP would be solved. The dark energy component is analyzed with both w= - 1 and w≠ - 1. Using Supernovae type Ia and Hubble parameter data constraints, in the case w= - 1 we find α=0.109-0.072+0.062 at 68% C.L., and the CP is alleviated. For w≠ - 1 , a degeneracy arises on the w–α plane. In order to break such degeneracy we add cosmic microwave background distance priors and baryonic acoustic oscillations data to the constraints, yielding α= - 0.075 ± 0.046 at 68% C.L. In this case we find that the CP is not alleviated even for 2σ interval for α. Furthermore, this last model is discarded against flat Λ CDM according to BIC analysis. |
publishDate |
2022 |
dc.date.none.fl_str_mv |
2022-04-29T08:41:25Z 2022-04-29T08:41:25Z 2022-03-01 |
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.uri.fl_str_mv |
http://dx.doi.org/10.1140/epjc/s10052-022-10234-y European Physical Journal C, v. 82, n. 3, 2022. 1434-6052 1434-6044 http://hdl.handle.net/11449/230664 10.1140/epjc/s10052-022-10234-y 2-s2.0-85127416496 |
url |
http://dx.doi.org/10.1140/epjc/s10052-022-10234-y http://hdl.handle.net/11449/230664 |
identifier_str_mv |
European Physical Journal C, v. 82, n. 3, 2022. 1434-6052 1434-6044 10.1140/epjc/s10052-022-10234-y 2-s2.0-85127416496 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
European Physical Journal C |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.source.none.fl_str_mv |
Scopus reponame:Repositório Institucional da UNESP instname:Universidade Estadual Paulista (UNESP) instacron:UNESP |
instname_str |
Universidade Estadual Paulista (UNESP) |
instacron_str |
UNESP |
institution |
UNESP |
reponame_str |
Repositório Institucional da UNESP |
collection |
Repositório Institucional da UNESP |
repository.name.fl_str_mv |
Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP) |
repository.mail.fl_str_mv |
|
_version_ |
1808128887087955968 |