Loading…

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...

Full description

Saved in:
Bibliographic Details
Published in:Astronomy and astrophysics (Berlin) 2015-12, Vol.584, p.A103
Main Authors: Sharma, B. K., Centelles, M., Viñas, X., Baldo, M., Burgio, G. F.
Format: Article
Language:English
Subjects:
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
cited_by cdi_FETCH-LOGICAL-c506t-24546bf5fbfff5b074c6331998d240339c54987689670c829cc0a9f7b2e4a2a63
cites cdi_FETCH-LOGICAL-c506t-24546bf5fbfff5b074c6331998d240339c54987689670c829cc0a9f7b2e4a2a63
container_end_page
container_issue
container_start_page A103
container_title Astronomy and astrophysics (Berlin)
container_volume 584
creator Sharma, B. K.
Centelles, M.
Viñas, X.
Baldo, M.
Burgio, G. F.
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.
doi_str_mv 10.1051/0004-6361/201526642
format article
fullrecord <record><control><sourceid>proquest_csuc_</sourceid><recordid>TN_cdi_csuc_recercat_oai_recercat_cat_2072_307242</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>1758355469</sourcerecordid><originalsourceid>FETCH-LOGICAL-c506t-24546bf5fbfff5b074c6331998d240339c54987689670c829cc0a9f7b2e4a2a63</originalsourceid><addsrcrecordid>eNqNkU1LAzEQhoMoWKu_wEuOXtbmO5ujLX5SEMXSY8imCUTbTZvsgv57s7TUq4dMMsP7hJl3ALjG6BYjjicIIVYJKvCEIMyJEIycgBFmlFRIMnEKRkfFObjI-bOkBNd0BKaLNvjgVtDtetOF2MLoYe5M56CPCbau71IplkrKsDwM3ASbYrZxGyxsTA75Epx5s87u6nCPweLh_mP2VM1fH59nd_PKciS6ijDOROO5b7z3vCl9WUEpVqpeEYYoVZYzVUtRKyGRrYmyFhnlZUMcM8QIOgZ4_6_NvdXJWZes6XQ04S8ZDkGSaFoCI4W52TPbFHe9y53ehGzdem1aF_ussZQ14kpK-Q8prykvM6gipYdOihM5Oa-3KWxM-tEY6WEherBbD3br40IKVe2pkDv3fURM-tJCUsl1jZb65V0g-rYkekp_AUKwil0</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>1758355469</pqid></control><display><type>article</type><title>Unified equation of state for neutron stars on a microscopic basis</title><source>EZB Electronic Journals Library</source><creator>Sharma, B. K. ; Centelles, M. ; Viñas, X. ; Baldo, M. ; Burgio, G. F.</creator><creatorcontrib>Sharma, B. K. ; Centelles, M. ; Viñas, X. ; Baldo, M. ; Burgio, G. F.</creatorcontrib><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.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/201526642</identifier><language>eng</language><publisher>EDP Sciences</publisher><subject>Asymptotic properties ; Computation ; Condensed matter ; Crusts ; dense matter ; Density ; Equacions d'estat ; equation of state ; Equations of state ; Estels de neutrons ; Mathematical models ; Matèria condensada ; Neutron stars ; Nuclei ; stars: neutron</subject><ispartof>Astronomy and astrophysics (Berlin), 2015-12, Vol.584, p.A103</ispartof><rights>(c) The European Southern Observatory (ESO), 2015 info:eu-repo/semantics/openAccess</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c506t-24546bf5fbfff5b074c6331998d240339c54987689670c829cc0a9f7b2e4a2a63</citedby><cites>FETCH-LOGICAL-c506t-24546bf5fbfff5b074c6331998d240339c54987689670c829cc0a9f7b2e4a2a63</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,780,784,885,27924,27925</link.rule.ids></links><search><creatorcontrib>Sharma, B. K.</creatorcontrib><creatorcontrib>Centelles, M.</creatorcontrib><creatorcontrib>Viñas, X.</creatorcontrib><creatorcontrib>Baldo, M.</creatorcontrib><creatorcontrib>Burgio, G. F.</creatorcontrib><title>Unified equation of state for neutron stars on a microscopic basis</title><title>Astronomy and astrophysics (Berlin)</title><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.</description><subject>Asymptotic properties</subject><subject>Computation</subject><subject>Condensed matter</subject><subject>Crusts</subject><subject>dense matter</subject><subject>Density</subject><subject>Equacions d'estat</subject><subject>equation of state</subject><subject>Equations of state</subject><subject>Estels de neutrons</subject><subject>Mathematical models</subject><subject>Matèria condensada</subject><subject>Neutron stars</subject><subject>Nuclei</subject><subject>stars: neutron</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2015</creationdate><recordtype>article</recordtype><recordid>eNqNkU1LAzEQhoMoWKu_wEuOXtbmO5ujLX5SEMXSY8imCUTbTZvsgv57s7TUq4dMMsP7hJl3ALjG6BYjjicIIVYJKvCEIMyJEIycgBFmlFRIMnEKRkfFObjI-bOkBNd0BKaLNvjgVtDtetOF2MLoYe5M56CPCbau71IplkrKsDwM3ASbYrZxGyxsTA75Epx5s87u6nCPweLh_mP2VM1fH59nd_PKciS6ijDOROO5b7z3vCl9WUEpVqpeEYYoVZYzVUtRKyGRrYmyFhnlZUMcM8QIOgZ4_6_NvdXJWZes6XQ04S8ZDkGSaFoCI4W52TPbFHe9y53ehGzdem1aF_ussZQ14kpK-Q8prykvM6gipYdOihM5Oa-3KWxM-tEY6WEherBbD3br40IKVe2pkDv3fURM-tJCUsl1jZb65V0g-rYkekp_AUKwil0</recordid><startdate>20151201</startdate><enddate>20151201</enddate><creator>Sharma, B. K.</creator><creator>Centelles, M.</creator><creator>Viñas, X.</creator><creator>Baldo, M.</creator><creator>Burgio, G. F.</creator><general>EDP Sciences</general><scope>BSCLL</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>XX2</scope></search><sort><creationdate>20151201</creationdate><title>Unified equation of state for neutron stars on a microscopic basis</title><author>Sharma, B. K. ; Centelles, M. ; Viñas, X. ; Baldo, M. ; Burgio, G. F.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c506t-24546bf5fbfff5b074c6331998d240339c54987689670c829cc0a9f7b2e4a2a63</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2015</creationdate><topic>Asymptotic properties</topic><topic>Computation</topic><topic>Condensed matter</topic><topic>Crusts</topic><topic>dense matter</topic><topic>Density</topic><topic>Equacions d'estat</topic><topic>equation of state</topic><topic>Equations of state</topic><topic>Estels de neutrons</topic><topic>Mathematical models</topic><topic>Matèria condensada</topic><topic>Neutron stars</topic><topic>Nuclei</topic><topic>stars: neutron</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Sharma, B. K.</creatorcontrib><creatorcontrib>Centelles, M.</creatorcontrib><creatorcontrib>Viñas, X.</creatorcontrib><creatorcontrib>Baldo, M.</creatorcontrib><creatorcontrib>Burgio, G. F.</creatorcontrib><collection>Istex</collection><collection>CrossRef</collection><collection>Meteorological &amp; Geoastrophysical Abstracts</collection><collection>Meteorological &amp; Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Recercat</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Sharma, B. K.</au><au>Centelles, M.</au><au>Viñas, X.</au><au>Baldo, M.</au><au>Burgio, G. F.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Unified equation of state for neutron stars on a microscopic basis</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2015-12-01</date><risdate>2015</risdate><volume>584</volume><spage>A103</spage><pages>A103-</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract>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.</abstract><pub>EDP Sciences</pub><doi>10.1051/0004-6361/201526642</doi><tpages>22</tpages><oa>free_for_read</oa></addata></record>
fulltext fulltext
identifier ISSN: 0004-6361
ispartof Astronomy and astrophysics (Berlin), 2015-12, Vol.584, p.A103
issn 0004-6361
1432-0746
language eng
recordid cdi_csuc_recercat_oai_recercat_cat_2072_307242
source EZB Electronic Journals Library
subjects Asymptotic properties
Computation
Condensed matter
Crusts
dense matter
Density
Equacions d'estat
equation of state
Equations of state
Estels de neutrons
Mathematical models
Matèria condensada
Neutron stars
Nuclei
stars: neutron
title Unified equation of state for neutron stars on a microscopic basis
url http://sfxeu10.hosted.exlibrisgroup.com/loughborough?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-25T11%3A50%3A19IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_csuc_&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Unified%20equation%20of%20state%20for%20neutron%20stars%20on%20a%20microscopic%20basis&rft.jtitle=Astronomy%20and%20astrophysics%20(Berlin)&rft.au=Sharma,%20B.%20K.&rft.date=2015-12-01&rft.volume=584&rft.spage=A103&rft.pages=A103-&rft.issn=0004-6361&rft.eissn=1432-0746&rft_id=info:doi/10.1051/0004-6361/201526642&rft_dat=%3Cproquest_csuc_%3E1758355469%3C/proquest_csuc_%3E%3Cgrp_id%3Ecdi_FETCH-LOGICAL-c506t-24546bf5fbfff5b074c6331998d240339c54987689670c829cc0a9f7b2e4a2a63%3C/grp_id%3E%3Coa%3E%3C/oa%3E%3Curl%3E%3C/url%3E&rft_id=info:oai/&rft_pqid=1758355469&rft_id=info:pmid/&rfr_iscdi=true