Neutron stars in accreting systems - Signatures of the QCD phase transition

Neutron stars (NS) that are born in binary systems with a main-sequence star companion can experience mass transfer, resulting in the accumulation of material at the surface of the NS. This, in turn, leads to the continuous growth of the NS mass and the associated steepening of the gravitational pot...

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Autores: Largani, NK, Fischer, T, Shibagaki, S, Cerdá-Durán, P, Torres-Forné, A
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2024
País:España
Institución:INCLIVA
Repositorio:r-INCLIVA. Repositorio Institucional de Producción Científica de INCLIVA
OAI Identifier:oai:incliva.fundanetsuite.com:p18510
Acceso en línea:https://incliva.portalinvestigacion.com/publicaciones/18510
Access Level:acceso abierto
Palabra clave:dense matter
equation of state
gravitational waves
neutrinos
stars: neutron
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spelling Neutron stars in accreting systems - Signatures of the QCD phase transitionLargani, NKFischer, TShibagaki, SCerdá-Durán, PTorres-Forné, Adense matterequation of stategravitational wavesneutrinosstars: neutronNeutron stars (NS) that are born in binary systems with a main-sequence star companion can experience mass transfer, resulting in the accumulation of material at the surface of the NS. This, in turn, leads to the continuous growth of the NS mass and the associated steepening of the gravitational potential. Supposing the central density surpasses the onset for the phase transition from nuclear, generally hadronic matter to deconfined quark-gluon plasma, which is a quantity currently constrained solely from an upper limit by asymptotic freedom in quantum chromodynamics (QCD), the system may experience a dynamic response due to the appearance of additional degrees of freedom in the equation of state (EOS). This dynamical response might give rise to a rapid softening of the EOS during the transition in the hadron-quark matter co-existence region. While this phenomenon has long been studied in the context of hydrostatic configurations, the dynamical implications of this problem are still incompletely understood. It is the purpose of the present paper to simulate the dynamics of NSs with previously accreted envelopes caused by the presence of a first-order QCD phase transition. Therefore, we employed the neutrino radiation hydrodynamics treatment based on the fully general relativistic approach in spherical symmetry, implementing a three-flavor Boltzmann neutrino transport and a microscopic model EOS that contains a first-order hadron-quark phase transition. The associated neutrino signal shows a sudden rise in the neutrino fluxes and average energies, becoming observable for the present generation of neutrino detectors for a galactic event, and a gravitational wave mode analysis revealed the behaviors of the dominant f mode and the first and the second gravity g modes that are excited during the NS evolution across the QCD phase transition.EDP SCIENCES S A2024info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttps://incliva.portalinvestigacion.com/publicaciones/18510ASTRONOMY & ASTROPHYSICSISSN: 00046361ISSNe: 14320746reponame:r-INCLIVA. Repositorio Institucional de Producción Científica de INCLIVAinstname:INCLIVAInglésinfo:eu-repo/semantics/openAccessoai:incliva.fundanetsuite.com:p185102026-06-07T16:35:31Z
dc.title.none.fl_str_mv Neutron stars in accreting systems - Signatures of the QCD phase transition
title Neutron stars in accreting systems - Signatures of the QCD phase transition
spellingShingle Neutron stars in accreting systems - Signatures of the QCD phase transition
Largani, NK
dense matter
equation of state
gravitational waves
neutrinos
stars: neutron
title_short Neutron stars in accreting systems - Signatures of the QCD phase transition
title_full Neutron stars in accreting systems - Signatures of the QCD phase transition
title_fullStr Neutron stars in accreting systems - Signatures of the QCD phase transition
title_full_unstemmed Neutron stars in accreting systems - Signatures of the QCD phase transition
title_sort Neutron stars in accreting systems - Signatures of the QCD phase transition
dc.creator.none.fl_str_mv Largani, NK
Fischer, T
Shibagaki, S
Cerdá-Durán, P
Torres-Forné, A
author Largani, NK
author_facet Largani, NK
Fischer, T
Shibagaki, S
Cerdá-Durán, P
Torres-Forné, A
author_role author
author2 Fischer, T
Shibagaki, S
Cerdá-Durán, P
Torres-Forné, A
author2_role author
author
author
author
dc.subject.none.fl_str_mv dense matter
equation of state
gravitational waves
neutrinos
stars: neutron
topic dense matter
equation of state
gravitational waves
neutrinos
stars: neutron
description Neutron stars (NS) that are born in binary systems with a main-sequence star companion can experience mass transfer, resulting in the accumulation of material at the surface of the NS. This, in turn, leads to the continuous growth of the NS mass and the associated steepening of the gravitational potential. Supposing the central density surpasses the onset for the phase transition from nuclear, generally hadronic matter to deconfined quark-gluon plasma, which is a quantity currently constrained solely from an upper limit by asymptotic freedom in quantum chromodynamics (QCD), the system may experience a dynamic response due to the appearance of additional degrees of freedom in the equation of state (EOS). This dynamical response might give rise to a rapid softening of the EOS during the transition in the hadron-quark matter co-existence region. While this phenomenon has long been studied in the context of hydrostatic configurations, the dynamical implications of this problem are still incompletely understood. It is the purpose of the present paper to simulate the dynamics of NSs with previously accreted envelopes caused by the presence of a first-order QCD phase transition. Therefore, we employed the neutrino radiation hydrodynamics treatment based on the fully general relativistic approach in spherical symmetry, implementing a three-flavor Boltzmann neutrino transport and a microscopic model EOS that contains a first-order hadron-quark phase transition. The associated neutrino signal shows a sudden rise in the neutrino fluxes and average energies, becoming observable for the present generation of neutrino detectors for a galactic event, and a gravitational wave mode analysis revealed the behaviors of the dominant f mode and the first and the second gravity g modes that are excited during the NS evolution across the QCD phase transition.
publishDate 2024
dc.date.none.fl_str_mv 2024
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://incliva.portalinvestigacion.com/publicaciones/18510
url https://incliva.portalinvestigacion.com/publicaciones/18510
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv EDP SCIENCES S A
publisher.none.fl_str_mv EDP SCIENCES S A
dc.source.none.fl_str_mv ASTRONOMY & ASTROPHYSICS
ISSN: 00046361
ISSNe: 14320746
reponame:r-INCLIVA. Repositorio Institucional de Producción Científica de INCLIVA
instname:INCLIVA
instname_str INCLIVA
reponame_str r-INCLIVA. Repositorio Institucional de Producción Científica de INCLIVA
collection r-INCLIVA. Repositorio Institucional de Producción Científica de INCLIVA
repository.name.fl_str_mv
repository.mail.fl_str_mv
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