3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: The magnetic field formalism

The long-term evolution of the internal, strong magnetic fields of neutron stars needs a specific numerical modelling. The diversity of the observed phenomenology of neutron stars indicates that their magnetic topology is rather complex and 3D simulations are required, for example, to explain the ob...

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Detalhes bibliográficos
Autores: Dehman, Clara, Viganò, Daniele, Pons, José A., Rea, Nanda
Tipo de documento: artigo
Estado:Versão publicada
Data de publicação:2023
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositório:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/336146
Acesso em linha:http://hdl.handle.net/10261/336146
Access Level:Acceso aberto
Palavra-chave:Stars: evolution
Stars: interiors
Stars: magnetars
Stars: magnetic field
Stars: neutron
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spelling 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: The magnetic field formalismDehman, ClaraViganò, DanielePons, José A.Rea, NandaStars: evolutionStars: interiorsStars: magnetarsStars: magnetic fieldStars: neutronThe long-term evolution of the internal, strong magnetic fields of neutron stars needs a specific numerical modelling. The diversity of the observed phenomenology of neutron stars indicates that their magnetic topology is rather complex and 3D simulations are required, for example, to explain the observed bursting mechanisms and the creation of surface hotspots. We present MATINS, a new 3D numerical code for magnetothermal evolution in neutron stars, based on a finite-volume scheme that employs the cubed-sphere system of coordinates. In this first work, we focus on the crustal magnetic evolution, with the inclusion of realistic calculations for the neutron star structure, composition, and electrical conductivity assuming a simple temperature evolution profile. MATINS follows the evolution of strong fields (1014 − 1015 Gauss) with complex non-axisymmetric topologies and dominant Hall-drift terms, and it is suitable for handling sharp current sheets. After introducing the technical description of our approach and some tests, we present long-term simulations of the non-linear field evolution in realistic neutron star crusts. The results show how the non-axisymmetric Hall cascade redistributes the energy over different spatial scales. Following the exploration of different initial topologies, we conclude that during a few tens of kyr, an equipartition of energy between the poloidal and toroidal components happens at small-scales. However, the magnetic field keeps a strong memory of the initial large scales, which are much harder to be restructured or created. This indicates that large-scale configuration attained during the neutron star formation is crucial to determine the field topology at any evolution stage.CD and NR are supported by the ERC Consolidator Grant ‘MAGNESIA’ No. 817661 (PI: Nanda Rea) and this work has been carried out within the framework of the doctoral program in Physics of the Universitat Autònoma de Barcelona. This work was also partially supported by the program Unidad de Excelencia María de Maeztu CEX2020-001058-M. 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 (PROMETEO/2019/071) and the AEI grant PID2021-127495NB-I00.With funding from the Spanish government through the ‘Severo Ochoa Centre of Excellence’ accreditation (CEX2020-001058-M).Peer reviewedOxford University PressEuropean CommissionEuropean Research CouncilUniversidad Autónoma de BarcelonaAgencia Estatal de Investigación (España)Ministerio de Ciencia, Innovación y Universidades (España)Generalitat ValencianaConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202320232023info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/336146reponame: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##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/EC/H2020/817661info:eu-repo/grantAgreement/AEI//CEX2020-001058-Minfo:eu-repo/grantAgreement/EC/H2020/948582info:eu-repo/grantAgreement/AEI//PID2021-127495NB-I00The underlying dataset has been published as supplementary material of the article in the publisher platform at DOI 10.1093/mnras/stac2761https://doi.org/10.1093/mnras/stac2761Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3361462026-05-22T06:33:51Z
dc.title.none.fl_str_mv 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: The magnetic field formalism
title 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: The magnetic field formalism
spellingShingle 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: The magnetic field formalism
Dehman, Clara
Stars: evolution
Stars: interiors
Stars: magnetars
Stars: magnetic field
Stars: neutron
title_short 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: The magnetic field formalism
title_full 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: The magnetic field formalism
title_fullStr 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: The magnetic field formalism
title_full_unstemmed 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: The magnetic field formalism
title_sort 3D code for MAgneto-Thermal evolution in Isolated Neutron Stars, MATINS: The magnetic field formalism
dc.creator.none.fl_str_mv Dehman, Clara
Viganò, Daniele
Pons, José A.
Rea, Nanda
author Dehman, Clara
author_facet Dehman, Clara
Viganò, Daniele
Pons, José A.
Rea, Nanda
author_role author
author2 Viganò, Daniele
Pons, José A.
Rea, Nanda
author2_role author
author
author
dc.contributor.none.fl_str_mv European Commission
European Research Council
Universidad Autónoma de Barcelona
Agencia Estatal de Investigación (España)
Ministerio de Ciencia, Innovación y Universidades (España)
Generalitat Valenciana
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 long-term evolution of the internal, strong magnetic fields of neutron stars needs a specific numerical modelling. The diversity of the observed phenomenology of neutron stars indicates that their magnetic topology is rather complex and 3D simulations are required, for example, to explain the observed bursting mechanisms and the creation of surface hotspots. We present MATINS, a new 3D numerical code for magnetothermal evolution in neutron stars, based on a finite-volume scheme that employs the cubed-sphere system of coordinates. In this first work, we focus on the crustal magnetic evolution, with the inclusion of realistic calculations for the neutron star structure, composition, and electrical conductivity assuming a simple temperature evolution profile. MATINS follows the evolution of strong fields (1014 − 1015 Gauss) with complex non-axisymmetric topologies and dominant Hall-drift terms, and it is suitable for handling sharp current sheets. After introducing the technical description of our approach and some tests, we present long-term simulations of the non-linear field evolution in realistic neutron star crusts. The results show how the non-axisymmetric Hall cascade redistributes the energy over different spatial scales. Following the exploration of different initial topologies, we conclude that during a few tens of kyr, an equipartition of energy between the poloidal and toroidal components happens at small-scales. However, the magnetic field keeps a strong memory of the initial large scales, which are much harder to be restructured or created. This indicates that large-scale configuration attained during the neutron star formation is crucial to determine the field topology at any evolution stage.
publishDate 2023
dc.date.none.fl_str_mv 2023
2023
2023
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/10261/336146
url http://hdl.handle.net/10261/336146
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#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/EC/H2020/817661
info:eu-repo/grantAgreement/AEI//CEX2020-001058-M
info:eu-repo/grantAgreement/EC/H2020/948582
info:eu-repo/grantAgreement/AEI//PID2021-127495NB-I00
The underlying dataset has been published as supplementary material of the article in the publisher platform at DOI 10.1093/mnras/stac2761
https://doi.org/10.1093/mnras/stac2761
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv 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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