Many-body forces in the equations of state of hyperonic matter
Autor(a) principal: | |
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Data de Publicação: | 2015 |
Outros Autores: | , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/126990 |
Resumo: | In this work we introduce an extended version of the formalism proposed originally by Taurines et al. that considers the effects of many-body forces simulated by nonlinear self-couplings and meson–meson interaction contributions. In this extended version of the model, we assume that matter is at zero temperature, charge neutral, and in beta-equilibrium, considering that the baryon octet interacts by the exchange of scalar–isoscalar (σ, s*), vector–isoscalar (ω, ϕ), vector–isovector ( ), and scalar–isovector (δ) meson fields. Using nuclear matter properties, we constrain the parameters of the model that describe the intensity of the indirectly density dependent baryon–meson couplings to a small range of possible values. We then investigate asymmetric hyperonic matter properties. We report that the formalism developed in this work is in reasonable agreement with experimental data and also allows for the existence of massive hyperon stars (with more than 2 M) with small radii, compatible with astrophysical observations. |
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Gomes, Rosana de OliveiraDexheimer, Veronica AntochevizSchramm, StefanVasconcellos, Cesar Augusto Zen2015-09-18T01:58:32Z20150004-637Xhttp://hdl.handle.net/10183/126990000973531In this work we introduce an extended version of the formalism proposed originally by Taurines et al. that considers the effects of many-body forces simulated by nonlinear self-couplings and meson–meson interaction contributions. In this extended version of the model, we assume that matter is at zero temperature, charge neutral, and in beta-equilibrium, considering that the baryon octet interacts by the exchange of scalar–isoscalar (σ, s*), vector–isoscalar (ω, ϕ), vector–isovector ( ), and scalar–isovector (δ) meson fields. Using nuclear matter properties, we constrain the parameters of the model that describe the intensity of the indirectly density dependent baryon–meson couplings to a small range of possible values. We then investigate asymmetric hyperonic matter properties. We report that the formalism developed in this work is in reasonable agreement with experimental data and also allows for the existence of massive hyperon stars (with more than 2 M) with small radii, compatible with astrophysical observations.application/pdfengThe astrophysical journal. Bristol. Vol. 808, no. 1 (July 2015), 8, 21 p.Massa estelarDimensões estelaresForcas nuclearesMatéria nuclearDensidade nuclearEquações de estadoDense matterEquation of stateStars: interiorsStars: neutronMany-body forces in the equations of state of hyperonic matterEstrangeiroinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFRGSinstname:Universidade Federal do Rio Grande do Sul (UFRGS)instacron:UFRGSORIGINAL000973531.pdf000973531.pdfTexto completo (inglês)application/pdf5230606http://www.lume.ufrgs.br/bitstream/10183/126990/1/000973531.pdf500764ececd561c2b22145b4faefd971MD51TEXT000973531.pdf.txt000973531.pdf.txtExtracted Texttext/plain93142http://www.lume.ufrgs.br/bitstream/10183/126990/2/000973531.pdf.txta6c648234f36bc163753ad9020f5f2a9MD52THUMBNAIL000973531.pdf.jpg000973531.pdf.jpgGenerated Thumbnailimage/jpeg2035http://www.lume.ufrgs.br/bitstream/10183/126990/3/000973531.pdf.jpg297fc9d5e79724e482d574d9648ad855MD5310183/1269902023-07-13 03:36:13.213117oai:www.lume.ufrgs.br:10183/126990Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-07-13T06:36:13Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Many-body forces in the equations of state of hyperonic matter |
title |
Many-body forces in the equations of state of hyperonic matter |
spellingShingle |
Many-body forces in the equations of state of hyperonic matter Gomes, Rosana de Oliveira Massa estelar Dimensões estelares Forcas nucleares Matéria nuclear Densidade nuclear Equações de estado Dense matter Equation of state Stars: interiors Stars: neutron |
title_short |
Many-body forces in the equations of state of hyperonic matter |
title_full |
Many-body forces in the equations of state of hyperonic matter |
title_fullStr |
Many-body forces in the equations of state of hyperonic matter |
title_full_unstemmed |
Many-body forces in the equations of state of hyperonic matter |
title_sort |
Many-body forces in the equations of state of hyperonic matter |
author |
Gomes, Rosana de Oliveira |
author_facet |
Gomes, Rosana de Oliveira Dexheimer, Veronica Antocheviz Schramm, Stefan Vasconcellos, Cesar Augusto Zen |
author_role |
author |
author2 |
Dexheimer, Veronica Antocheviz Schramm, Stefan Vasconcellos, Cesar Augusto Zen |
author2_role |
author author author |
dc.contributor.author.fl_str_mv |
Gomes, Rosana de Oliveira Dexheimer, Veronica Antocheviz Schramm, Stefan Vasconcellos, Cesar Augusto Zen |
dc.subject.por.fl_str_mv |
Massa estelar Dimensões estelares Forcas nucleares Matéria nuclear Densidade nuclear Equações de estado |
topic |
Massa estelar Dimensões estelares Forcas nucleares Matéria nuclear Densidade nuclear Equações de estado Dense matter Equation of state Stars: interiors Stars: neutron |
dc.subject.eng.fl_str_mv |
Dense matter Equation of state Stars: interiors Stars: neutron |
description |
In this work we introduce an extended version of the formalism proposed originally by Taurines et al. that considers the effects of many-body forces simulated by nonlinear self-couplings and meson–meson interaction contributions. In this extended version of the model, we assume that matter is at zero temperature, charge neutral, and in beta-equilibrium, considering that the baryon octet interacts by the exchange of scalar–isoscalar (σ, s*), vector–isoscalar (ω, ϕ), vector–isovector ( ), and scalar–isovector (δ) meson fields. Using nuclear matter properties, we constrain the parameters of the model that describe the intensity of the indirectly density dependent baryon–meson couplings to a small range of possible values. We then investigate asymmetric hyperonic matter properties. We report that the formalism developed in this work is in reasonable agreement with experimental data and also allows for the existence of massive hyperon stars (with more than 2 M) with small radii, compatible with astrophysical observations. |
publishDate |
2015 |
dc.date.accessioned.fl_str_mv |
2015-09-18T01:58:32Z |
dc.date.issued.fl_str_mv |
2015 |
dc.type.driver.fl_str_mv |
Estrangeiro info:eu-repo/semantics/article |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
format |
article |
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publishedVersion |
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http://hdl.handle.net/10183/126990 |
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0004-637X |
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000973531 |
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http://hdl.handle.net/10183/126990 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
The astrophysical journal. Bristol. Vol. 808, no. 1 (July 2015), 8, 21 p. |
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info:eu-repo/semantics/openAccess |
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openAccess |
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