3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: thermal evolution and light curves

The thermal evolution of isolated neutron stars is a key element in unraveling their internal structure and composition and establishing evolutionary connections among different observational subclasses. Previous studies have predominantly focused on one-dimensional or axisymmetric two-dimensional m...

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Detalles Bibliográficos
Autores: Ascenzi, Stefano, Viganò, Daniele, Dehman, Clara, Pons, José A., Rea, Nanda, Perna, Rosalba
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2024
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/377864
Acceso en línea:http://hdl.handle.net/10261/377864
http://arxiv.org/abs/2401.15711v2
Access Level:acceso abierto
Palabra clave:Stars: evolution
Stars: interiors
Stars: magnetars
Stars: magnetic field
Stars: neutron
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oai_identifier_str oai:digital.csic.es:10261/377864
network_acronym_str ES
network_name_str España
repository_id_str
dc.title.none.fl_str_mv 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: thermal evolution and light curves
title 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: thermal evolution and light curves
spellingShingle 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: thermal evolution and light curves
Ascenzi, Stefano
Stars: evolution
Stars: interiors
Stars: magnetars
Stars: magnetic field
Stars: neutron
title_short 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: thermal evolution and light curves
title_full 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: thermal evolution and light curves
title_fullStr 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: thermal evolution and light curves
title_full_unstemmed 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: thermal evolution and light curves
title_sort 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: thermal evolution and light curves
dc.creator.none.fl_str_mv Ascenzi, Stefano
Viganò, Daniele
Dehman, Clara
Pons, José A.
Rea, Nanda
Perna, Rosalba
author Ascenzi, Stefano
author_facet Ascenzi, Stefano
Viganò, Daniele
Dehman, Clara
Pons, José A.
Rea, Nanda
Perna, Rosalba
author_role author
author2 Viganò, Daniele
Dehman, Clara
Pons, José A.
Rea, Nanda
Perna, Rosalba
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv European Research Council
European Commission
Generalitat Valenciana
Agencia Estatal de Investigación (España)
Universidad Autónoma de Barcelona
National Science Foundation (US)
Rea, Nanda [0000-0003-2177-6388]
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Stars: evolution
Stars: interiors
Stars: magnetars
Stars: magnetic field
Stars: neutron
topic Stars: evolution
Stars: interiors
Stars: magnetars
Stars: magnetic field
Stars: neutron
description The thermal evolution of isolated neutron stars is a key element in unraveling their internal structure and composition and establishing evolutionary connections among different observational subclasses. Previous studies have predominantly focused on one-dimensional or axisymmetric two-dimensional models. In this study, we present the thermal evolution component of the novel three-dimensional magnetothermal code MATINS (MAgneto-Thermal evolution of Isolated Neutron Star). MATINS employs a finite volume scheme and integrates a realistic background structure, along with state-of-the-art microphysical calculations for the conductivities, neutrino emissivities, heat capacity, and superfluid gap models. This paper outlines the methodology employed to solve the thermal evolution equations in MATINS, along with the microphysical implementation which is essential for the thermal component. We test the accuracy of the code and present simulations with non-evolving magnetic fields of different configurations (all with electrical currents confined to the crust and a magnetic field that does not thread the core), to produce temperature maps of the neutron star surface. Additionally, for a specific magnetic field configuration, we show one fully coupled evolution of magnetic field and temperature. Subsequently, we use a ray-tracing code to link the neutron star surface temperature maps obtained by MATINS with the phase-resolved spectra and pulsed profiles that would be detected by distant observers. This study, together with our previous article focused on the magnetic formalism, presents in detail the most advanced evolutionary code for isolated neutron stars, with the aim of comparison with their timing properties, thermal luminosities and the associated X-ray light curves.
publishDate 2024
dc.date.none.fl_str_mv 2024
2025
2025
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/377864
http://arxiv.org/abs/2401.15711v2
url http://hdl.handle.net/10261/377864
http://arxiv.org/abs/2401.15711v2
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu‐repo/grantAgreement/EC/H2020/817661
info:eu‐repo/grantAgreement/EC/H2020/948582
info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/PID2021-127495NB-I00
https://doi.org/10.1093/mnras/stae1749
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv Royal Astronomical Society
Oxford University Press
publisher.none.fl_str_mv Royal Astronomical Society
Oxford University Press
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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spelling 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: thermal evolution and light curvesAscenzi, StefanoViganò, DanieleDehman, ClaraPons, José A.Rea, NandaPerna, RosalbaStars: evolutionStars: interiorsStars: magnetarsStars: magnetic fieldStars: neutronThe thermal evolution of isolated neutron stars is a key element in unraveling their internal structure and composition and establishing evolutionary connections among different observational subclasses. Previous studies have predominantly focused on one-dimensional or axisymmetric two-dimensional models. In this study, we present the thermal evolution component of the novel three-dimensional magnetothermal code MATINS (MAgneto-Thermal evolution of Isolated Neutron Star). MATINS employs a finite volume scheme and integrates a realistic background structure, along with state-of-the-art microphysical calculations for the conductivities, neutrino emissivities, heat capacity, and superfluid gap models. This paper outlines the methodology employed to solve the thermal evolution equations in MATINS, along with the microphysical implementation which is essential for the thermal component. We test the accuracy of the code and present simulations with non-evolving magnetic fields of different configurations (all with electrical currents confined to the crust and a magnetic field that does not thread the core), to produce temperature maps of the neutron star surface. Additionally, for a specific magnetic field configuration, we show one fully coupled evolution of magnetic field and temperature. Subsequently, we use a ray-tracing code to link the neutron star surface temperature maps obtained by MATINS with the phase-resolved spectra and pulsed profiles that would be detected by distant observers. This study, together with our previous article focused on the magnetic formalism, presents in detail the most advanced evolutionary code for isolated neutron stars, with the aim of comparison with their timing properties, thermal luminosities and the associated X-ray light curves.SA, NR, and CD are supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (ERC Consolidator Grant ‘MAGNESIA’ No. 817661, PI: NR), and acknowledge partial support from grant SGR2021-01269 (PI: Graber/Rea). CD acknowledges the Nordita Visiting PhD Fellow programme. DV is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (ERC Starting Grant ‘IMAGINE’ No. 948582, PI: DV). JAP acknowledges support from the Generalitat Valenciana grants ASFAE/2022/026 (with funding from NextGenerationEU PRTR-C17.I1) and the AEI grant PID2021-127495NB-I00. SA, DV, CD, and NR acknowledge support from ‘María de Maeztu’ award to the Institut de Ciències de l’Espai (CEX2020-001058-M). RP acknowledges support by NSF award AST-2006839. CD’s work has been carried out within the framework of the doctoral programme in Physics of the Universitat Autónoma de Barcelona. We thank Carlos Palenzuela and Borja Miñano (UIB-IAC3) for the computational support. We thank Davide de Grandis for the useful discussions. The authors acknowledges the anonymous referee for the suggestions that help us to improve the presentation of our manuscript.Peer reviewedRoyal Astronomical SocietyOxford University PressEuropean Research CouncilEuropean CommissionGeneralitat ValencianaAgencia Estatal de Investigación (España)Universidad Autónoma de BarcelonaNational Science Foundation (US)Rea, Nanda [0000-0003-2177-6388]Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202520252024info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/377864http://arxiv.org/abs/2401.15711v2reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu‐repo/grantAgreement/EC/H2020/817661info:eu‐repo/grantAgreement/EC/H2020/948582info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/PID2021-127495NB-I00https://doi.org/10.1093/mnras/stae1749Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3778642026-05-22T06:33:51Z
score 15,812429

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