Unified equation of state for neutron stars on a microscopic basis

We derive a new equation of state (EoS) for neutron stars (NS) from the outer crust to the core based on modern microscopic calculations using the Argonne v18 potential plus three-body forces computed with the Urbana model. To deal with the inhomogeneous structures of matter in the NS crust, we use...

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Autores: Sharma, B. K., Centelles Aixalà, Mario, Viñas Gausí, Xavier, Baldo, M., Burgio, G. M.
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2015
País:España
Recursos:Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya)
Repositorio:Recercat. Dipósit de la Recerca de Catalunya
OAI Identifier:oai:recercat.cat:2445/121321
Acesso em linha:https://hdl.handle.net/2445/121321
Access Level:acceso abierto
Palavra-chave:Equacions d'estat
Estels de neutrons
Matèria condensada
Equations of state
Neutron stars
Condensed matter
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spelling Unified equation of state for neutron stars on a microscopic basisSharma, B. K.Centelles Aixalà, MarioViñas Gausí, XavierBaldo, M.Burgio, G. M.Equacions d'estatEstels de neutronsMatèria condensadaEquations of stateNeutron starsCondensed matterWe derive a new equation of state (EoS) for neutron stars (NS) from the outer crust to the core based on modern microscopic calculations using the Argonne v18 potential plus three-body forces computed with the Urbana model. To deal with the inhomogeneous structures of matter in the NS crust, we use a recent nuclear energy density functional that is directly based on the same microscopic calculations, and which is able to reproduce the ground-state properties of nuclei along the periodic table. The EoS of the outer crust requires the masses of neutron-rich nuclei, which are obtained through Hartree-Fock-Bogoliubov calculations with the new functional when they are unknown experimentally. To compute the inner crust, Thomas-Fermi calculations in Wigner-Seitz cells are performed with the same functional. Existence of nuclear pasta is predicted in a range of average baryon densities between 0.067 fm−3 and 0.0825 fm−3, where the transition to the core takes place. The NS core is computed from the new nuclear EoS assuming non-exotic constituents (core of npeμ matter). In each region of the star, we discuss the comparison of the new EoS with previous EoSs for the complete NS structure, widely used in astrophysical calculations. The new microscopically derived EoS fulfills at the same time a NS maximum mass of 2 M with a radius of 10 km, and a 1.5 M NS with a radius of 11.6 km.EDP Sciences2018201820152018info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersion22 p.application/pdfhttps://hdl.handle.net/2445/121321Articles publicats en revistes (Física Quàntica i Astrofísica)reponame:Recercat. Dipósit de la Recerca de Catalunyainstname:Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya)InglésReproducció del document publicat a: https://doi.org/10.1051/0004-6361/201526642Astronomy & Astrophysics, 2015, vol. 584, p. A103https://doi.org/10.1051/0004-6361/201526642(c) The European Southern Observatory (ESO), 2015info:eu-repo/semantics/openAccessoai:recercat.cat:2445/1213212026-05-29T05:05:01Z
dc.title.none.fl_str_mv Unified equation of state for neutron stars on a microscopic basis
title Unified equation of state for neutron stars on a microscopic basis
spellingShingle Unified equation of state for neutron stars on a microscopic basis
Sharma, B. K.
Equacions d'estat
Estels de neutrons
Matèria condensada
Equations of state
Neutron stars
Condensed matter
title_short Unified equation of state for neutron stars on a microscopic basis
title_full Unified equation of state for neutron stars on a microscopic basis
title_fullStr Unified equation of state for neutron stars on a microscopic basis
title_full_unstemmed Unified equation of state for neutron stars on a microscopic basis
title_sort Unified equation of state for neutron stars on a microscopic basis
dc.creator.none.fl_str_mv Sharma, B. K.
Centelles Aixalà, Mario
Viñas Gausí, Xavier
Baldo, M.
Burgio, G. M.
author Sharma, B. K.
author_facet Sharma, B. K.
Centelles Aixalà, Mario
Viñas Gausí, Xavier
Baldo, M.
Burgio, G. M.
author_role author
author2 Centelles Aixalà, Mario
Viñas Gausí, Xavier
Baldo, M.
Burgio, G. M.
author2_role author
author
author
author
dc.subject.none.fl_str_mv Equacions d'estat
Estels de neutrons
Matèria condensada
Equations of state
Neutron stars
Condensed matter
topic Equacions d'estat
Estels de neutrons
Matèria condensada
Equations of state
Neutron stars
Condensed matter
description We derive a new equation of state (EoS) for neutron stars (NS) from the outer crust to the core based on modern microscopic calculations using the Argonne v18 potential plus three-body forces computed with the Urbana model. To deal with the inhomogeneous structures of matter in the NS crust, we use a recent nuclear energy density functional that is directly based on the same microscopic calculations, and which is able to reproduce the ground-state properties of nuclei along the periodic table. The EoS of the outer crust requires the masses of neutron-rich nuclei, which are obtained through Hartree-Fock-Bogoliubov calculations with the new functional when they are unknown experimentally. To compute the inner crust, Thomas-Fermi calculations in Wigner-Seitz cells are performed with the same functional. Existence of nuclear pasta is predicted in a range of average baryon densities between 0.067 fm−3 and 0.0825 fm−3, where the transition to the core takes place. The NS core is computed from the new nuclear EoS assuming non-exotic constituents (core of npeμ matter). In each region of the star, we discuss the comparison of the new EoS with previous EoSs for the complete NS structure, widely used in astrophysical calculations. The new microscopically derived EoS fulfills at the same time a NS maximum mass of 2 M with a radius of 10 km, and a 1.5 M NS with a radius of 11.6 km.
publishDate 2015
dc.date.none.fl_str_mv 2015
2018
2018
2018
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv https://hdl.handle.net/2445/121321
url https://hdl.handle.net/2445/121321
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv Reproducció del document publicat a: https://doi.org/10.1051/0004-6361/201526642
Astronomy & Astrophysics, 2015, vol. 584, p. A103
https://doi.org/10.1051/0004-6361/201526642
dc.rights.none.fl_str_mv (c) The European Southern Observatory (ESO), 2015
info:eu-repo/semantics/openAccess
rights_invalid_str_mv (c) The European Southern Observatory (ESO), 2015
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv 22 p.
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv Articles publicats en revistes (Física Quàntica i Astrofísica)
reponame:Recercat. Dipósit de la Recerca de Catalunya
instname:Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya)
instname_str Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya)
reponame_str Recercat. Dipósit de la Recerca de Catalunya
collection Recercat. Dipósit de la Recerca de Catalunya
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15.811543

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