Effects of the quark-hadron phase transition on highly magnetized neutron stars
Autor(a) principal: | |
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Data de Publicação: | 2016 |
Outros Autores: | , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/150358 |
Resumo: | The presence of quark-hadron phase transitions in neutron stars can be related to several interesting phenomena. In particular, previous calculations have shown that fast rotating neutron stars, when subjected to a quark-hadron phase transition in their interiors, could give rise to the backbending phenomenon characterized by a spin-up era. In this work, we use an equation of state composed of two phases, containing nucleons (and leptons) and quarks. The hadronic phase is described in a relativistic mean field formalism that takes many-body forces into account, and the quark phase is described by the MIT bag model with a vector interaction. Stationary and axisymmetric stellar models are obtained in a self-consistent way by solving numerically the Einstein–Maxwell equations by means of a pseudo-spectral method. As a result, we obtain the interesting backbending phenomenon for fast spinning neutron stars. More importantly, we show that a magnetic field, which is assumed to be axisymmetric and poloidal, can also be enhanced due to the phase transition from normal hadronic matter to quark matter on highly magnetized neutron stars. Therefore, in parallel to the spin-up era, classes of neutron stars endowed with strong magnetic fields may go through a ‘magnetic-up era’ in their lives. |
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Franzon, BrunoGomes, Rosana de OliveiraSchramm, Stefan2016-12-31T02:20:59Z20160035-8711http://hdl.handle.net/10183/150358001008156The presence of quark-hadron phase transitions in neutron stars can be related to several interesting phenomena. In particular, previous calculations have shown that fast rotating neutron stars, when subjected to a quark-hadron phase transition in their interiors, could give rise to the backbending phenomenon characterized by a spin-up era. In this work, we use an equation of state composed of two phases, containing nucleons (and leptons) and quarks. The hadronic phase is described in a relativistic mean field formalism that takes many-body forces into account, and the quark phase is described by the MIT bag model with a vector interaction. Stationary and axisymmetric stellar models are obtained in a self-consistent way by solving numerically the Einstein–Maxwell equations by means of a pseudo-spectral method. As a result, we obtain the interesting backbending phenomenon for fast spinning neutron stars. More importantly, we show that a magnetic field, which is assumed to be axisymmetric and poloidal, can also be enhanced due to the phase transition from normal hadronic matter to quark matter on highly magnetized neutron stars. Therefore, in parallel to the spin-up era, classes of neutron stars endowed with strong magnetic fields may go through a ‘magnetic-up era’ in their lives.application/pdfengMonthly notices of the Royal Astronomical Society. Oxford. Vol. 463, no. 1 (Nov. 2016), p. 571-579Ondas gravitacionaisCampos magnéticosEquações de estadoEstrelas de neutronsEquation of stateGravitational wavesMagnetic fieldsEffects of the quark-hadron phase transition on highly magnetized neutron starsEstrangeiroinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFRGSinstname:Universidade Federal do Rio Grande do Sul (UFRGS)instacron:UFRGSORIGINAL001008156.pdf001008156.pdfTexto completo (inglês)application/pdf611929http://www.lume.ufrgs.br/bitstream/10183/150358/1/001008156.pdf114fbf1f4061a38228ad14e12c3b43c4MD51TEXT001008156.pdf.txt001008156.pdf.txtExtracted Texttext/plain51371http://www.lume.ufrgs.br/bitstream/10183/150358/2/001008156.pdf.txt4fcc66bf131d8b382e34363b9d8444d7MD52THUMBNAIL001008156.pdf.jpg001008156.pdf.jpgGenerated Thumbnailimage/jpeg2148http://www.lume.ufrgs.br/bitstream/10183/150358/3/001008156.pdf.jpgc8408169c9c76ffb752e41e9eb9b42edMD5310183/1503582018-10-30 07:56:53.694oai:www.lume.ufrgs.br:10183/150358Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2018-10-30T10:56:53Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Effects of the quark-hadron phase transition on highly magnetized neutron stars |
title |
Effects of the quark-hadron phase transition on highly magnetized neutron stars |
spellingShingle |
Effects of the quark-hadron phase transition on highly magnetized neutron stars Franzon, Bruno Ondas gravitacionais Campos magnéticos Equações de estado Estrelas de neutrons Equation of state Gravitational waves Magnetic fields |
title_short |
Effects of the quark-hadron phase transition on highly magnetized neutron stars |
title_full |
Effects of the quark-hadron phase transition on highly magnetized neutron stars |
title_fullStr |
Effects of the quark-hadron phase transition on highly magnetized neutron stars |
title_full_unstemmed |
Effects of the quark-hadron phase transition on highly magnetized neutron stars |
title_sort |
Effects of the quark-hadron phase transition on highly magnetized neutron stars |
author |
Franzon, Bruno |
author_facet |
Franzon, Bruno Gomes, Rosana de Oliveira Schramm, Stefan |
author_role |
author |
author2 |
Gomes, Rosana de Oliveira Schramm, Stefan |
author2_role |
author author |
dc.contributor.author.fl_str_mv |
Franzon, Bruno Gomes, Rosana de Oliveira Schramm, Stefan |
dc.subject.por.fl_str_mv |
Ondas gravitacionais Campos magnéticos Equações de estado Estrelas de neutrons |
topic |
Ondas gravitacionais Campos magnéticos Equações de estado Estrelas de neutrons Equation of state Gravitational waves Magnetic fields |
dc.subject.eng.fl_str_mv |
Equation of state Gravitational waves Magnetic fields |
description |
The presence of quark-hadron phase transitions in neutron stars can be related to several interesting phenomena. In particular, previous calculations have shown that fast rotating neutron stars, when subjected to a quark-hadron phase transition in their interiors, could give rise to the backbending phenomenon characterized by a spin-up era. In this work, we use an equation of state composed of two phases, containing nucleons (and leptons) and quarks. The hadronic phase is described in a relativistic mean field formalism that takes many-body forces into account, and the quark phase is described by the MIT bag model with a vector interaction. Stationary and axisymmetric stellar models are obtained in a self-consistent way by solving numerically the Einstein–Maxwell equations by means of a pseudo-spectral method. As a result, we obtain the interesting backbending phenomenon for fast spinning neutron stars. More importantly, we show that a magnetic field, which is assumed to be axisymmetric and poloidal, can also be enhanced due to the phase transition from normal hadronic matter to quark matter on highly magnetized neutron stars. Therefore, in parallel to the spin-up era, classes of neutron stars endowed with strong magnetic fields may go through a ‘magnetic-up era’ in their lives. |
publishDate |
2016 |
dc.date.accessioned.fl_str_mv |
2016-12-31T02:20:59Z |
dc.date.issued.fl_str_mv |
2016 |
dc.type.driver.fl_str_mv |
Estrangeiro info:eu-repo/semantics/article |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
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article |
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publishedVersion |
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http://hdl.handle.net/10183/150358 |
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0035-8711 |
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001008156 |
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http://hdl.handle.net/10183/150358 |
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eng |
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eng |
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Monthly notices of the Royal Astronomical Society. Oxford. Vol. 463, no. 1 (Nov. 2016), p. 571-579 |
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openAccess |
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