Color superconductivity in compact stellar hybrid configurations

Autores
Ranea Sandoval, Ignacio Francisco; Orsaria, Milva Gabriela; Han, Sophia; Weber, Fridolin; Spinella, William M.
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The discovery of pulsars PSR J1614-2230 and PSR J0348+0432 with masses of around 2Mʘ imposes strong constraints on the equations of state of cold, ultradense matter. If a phase transition from hadronic matter to quark matter were to occur in the inner cores of such massive neutron stars, the energetically favorable state of quark matter would be a color superconductor. In this study, we analyze the stability and maximum mass of such neutron stars. The hadronic phase is described by nonlinear relativistic mean-field models, and the local Nambu-Jona Lasinio model is used to describe quark matter in the 2SC+s quark phase. The phase transition is treated as a Maxwell transition, assuming a sharp hadron-quark interface, and the "constant-sound-speed" (CSS) parametrization is employed to discuss the existence of stellar twin configurations. We find that massive neutron stars such as J1614-2230 and J0348+0432 can only exist on the connected stellar branch but not on the disconnected twin-star branch. The latter can only support stars with masses that are strictly below 2Mʘ.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
Nuclear matter in neutron stars
Asymmetric nuclear matter
Equations of state of nuclear matter
Nuclear astrophysics
Neutron stars
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/87239
Acceder
id SEDICI_9592568d6b60eccc9873b968b6968fb3
oai_identifier_str oai:sedici.unlp.edu.ar:10915/87239
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Color superconductivity in compact stellar hybrid configurationsRanea Sandoval, Ignacio FranciscoOrsaria, Milva GabrielaHan, SophiaWeber, FridolinSpinella, William M.Ciencias AstronómicasNuclear matter in neutron starsAsymmetric nuclear matterEquations of state of nuclear matterNuclear astrophysicsNeutron starsThe discovery of pulsars PSR J1614-2230 and PSR J0348+0432 with masses of around 2M<sub>ʘ</sub> imposes strong constraints on the equations of state of cold, ultradense matter. If a phase transition from hadronic matter to quark matter were to occur in the inner cores of such massive neutron stars, the energetically favorable state of quark matter would be a color superconductor. In this study, we analyze the stability and maximum mass of such neutron stars. The hadronic phase is described by nonlinear relativistic mean-field models, and the local Nambu-Jona Lasinio model is used to describe quark matter in the 2SC+s quark phase. The phase transition is treated as a Maxwell transition, assuming a sharp hadron-quark interface, and the "constant-sound-speed" (CSS) parametrization is employed to discuss the existence of stellar twin configurations. We find that massive neutron stars such as J1614-2230 and J0348+0432 can only exist on the connected stellar branch but not on the disconnected twin-star branch. The latter can only support stars with masses that are strictly below 2M<sub>ʘ</sub>.Facultad de Ciencias Astronómicas y Geofísicas2017-12-29info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/87239enginfo:eu-repo/semantics/altIdentifier/issn/2469-9985info:eu-repo/semantics/altIdentifier/doi/10.1103/PhysRevC.96.065807info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/4.0/Creative Commons Attribution 4.0 International (CC BY 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-10-15T11:09:02Zoai:sedici.unlp.edu.ar:10915/87239Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-10-15 11:09:03.041SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Color superconductivity in compact stellar hybrid configurations
title Color superconductivity in compact stellar hybrid configurations
spellingShingle Color superconductivity in compact stellar hybrid configurations
Ranea Sandoval, Ignacio Francisco
Ciencias Astronómicas
Nuclear matter in neutron stars
Asymmetric nuclear matter
Equations of state of nuclear matter
Nuclear astrophysics
Neutron stars
title_short Color superconductivity in compact stellar hybrid configurations
title_full Color superconductivity in compact stellar hybrid configurations
title_fullStr Color superconductivity in compact stellar hybrid configurations
title_full_unstemmed Color superconductivity in compact stellar hybrid configurations
title_sort Color superconductivity in compact stellar hybrid configurations
dc.creator.none.fl_str_mv Ranea Sandoval, Ignacio Francisco
Orsaria, Milva Gabriela
Han, Sophia
Weber, Fridolin
Spinella, William M.
author Ranea Sandoval, Ignacio Francisco
author_facet Ranea Sandoval, Ignacio Francisco
Orsaria, Milva Gabriela
Han, Sophia
Weber, Fridolin
Spinella, William M.
author_role author
author2 Orsaria, Milva Gabriela
Han, Sophia
Weber, Fridolin
Spinella, William M.
author2_role author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Nuclear matter in neutron stars
Asymmetric nuclear matter
Equations of state of nuclear matter
Nuclear astrophysics
Neutron stars
topic Ciencias Astronómicas
Nuclear matter in neutron stars
Asymmetric nuclear matter
Equations of state of nuclear matter
Nuclear astrophysics
Neutron stars
dc.description.none.fl_txt_mv The discovery of pulsars PSR J1614-2230 and PSR J0348+0432 with masses of around 2M<sub>ʘ</sub> imposes strong constraints on the equations of state of cold, ultradense matter. If a phase transition from hadronic matter to quark matter were to occur in the inner cores of such massive neutron stars, the energetically favorable state of quark matter would be a color superconductor. In this study, we analyze the stability and maximum mass of such neutron stars. The hadronic phase is described by nonlinear relativistic mean-field models, and the local Nambu-Jona Lasinio model is used to describe quark matter in the 2SC+s quark phase. The phase transition is treated as a Maxwell transition, assuming a sharp hadron-quark interface, and the "constant-sound-speed" (CSS) parametrization is employed to discuss the existence of stellar twin configurations. We find that massive neutron stars such as J1614-2230 and J0348+0432 can only exist on the connected stellar branch but not on the disconnected twin-star branch. The latter can only support stars with masses that are strictly below 2M<sub>ʘ</sub>.
Facultad de Ciencias Astronómicas y Geofísicas
description The discovery of pulsars PSR J1614-2230 and PSR J0348+0432 with masses of around 2M<sub>ʘ</sub> imposes strong constraints on the equations of state of cold, ultradense matter. If a phase transition from hadronic matter to quark matter were to occur in the inner cores of such massive neutron stars, the energetically favorable state of quark matter would be a color superconductor. In this study, we analyze the stability and maximum mass of such neutron stars. The hadronic phase is described by nonlinear relativistic mean-field models, and the local Nambu-Jona Lasinio model is used to describe quark matter in the 2SC+s quark phase. The phase transition is treated as a Maxwell transition, assuming a sharp hadron-quark interface, and the "constant-sound-speed" (CSS) parametrization is employed to discuss the existence of stellar twin configurations. We find that massive neutron stars such as J1614-2230 and J0348+0432 can only exist on the connected stellar branch but not on the disconnected twin-star branch. The latter can only support stars with masses that are strictly below 2M<sub>ʘ</sub>.
publishDate 2017
dc.date.none.fl_str_mv 2017-12-29
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/87239
url http://sedici.unlp.edu.ar/handle/10915/87239
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/2469-9985
info:eu-repo/semantics/altIdentifier/doi/10.1103/PhysRevC.96.065807
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/4.0/
Creative Commons Attribution 4.0 International (CC BY 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/4.0/
Creative Commons Attribution 4.0 International (CC BY 4.0)
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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score 13.22299

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