Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interface

Autores
Mariani, Mauro; Orsaria, Milva Gabriela; Ranea Sandoval, Ignacio Francisco; Lugones, Germán
Año de publicación
2019
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We study the influence of strong magnetic fields in hybrid stars, composed by hadrons and a pure quark matter core, and analyse their structure and stability as well as some possible evolution channels due to the magnetic field decay. Using an ad hoc parametrization of the magnetic field strength and taking into account Landau-quantization effects in matter, we calculate hybrid magnetized equations of state and some associated quantities, such as particle abundances and matter magnetization, for different sets of parameters and different magnetic field strengths. Moreover, we compute the magnetized stable stellar configurations, the mass versus radius and the gravitational mass versus central energy density relationships, the gravitational mass versus baryon mass diagram, and the tidal deformability. Our results are in agreement with both, the∼ 2 M¯ pulsars and the data obtained from GW170817. In addition, we study the stability of stellar configurations assuming that slow and rapid phase transitions occur at the sharp hadron–quark interface. We find that, unlike in the rapid transition scenario, where ∂M/∂²c < 0 is a sufficient condition for instability, in the slow transition scenario there exists a connected extended stable branch beyond the maximum mass star, for which ∂M/∂²c < 0. Finally, analysing the gravitational mass versus baryon mass relationship, we have calculated the energy released in transitions between stable stellar configurations. We find that the inclusion of the magnetic field and the existence of new stable branches allows the possibility of new channels of transitions that fulfil the energy requirements to explain gamma-ray bursts.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
Dense matter
equation of state
stars: magnetars
stars: neutron
stars: oscillations
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/126594

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/126594
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interfaceMariani, MauroOrsaria, Milva GabrielaRanea Sandoval, Ignacio FranciscoLugones, GermánCiencias AstronómicasDense matterequation of statestars: magnetarsstars: neutronstars: oscillationsWe study the influence of strong magnetic fields in hybrid stars, composed by hadrons and a pure quark matter core, and analyse their structure and stability as well as some possible evolution channels due to the magnetic field decay. Using an ad hoc parametrization of the magnetic field strength and taking into account Landau-quantization effects in matter, we calculate hybrid magnetized equations of state and some associated quantities, such as particle abundances and matter magnetization, for different sets of parameters and different magnetic field strengths. Moreover, we compute the magnetized stable stellar configurations, the mass versus radius and the gravitational mass versus central energy density relationships, the gravitational mass versus baryon mass diagram, and the tidal deformability. Our results are in agreement with both, the∼ 2 M¯ pulsars and the data obtained from GW170817. In addition, we study the stability of stellar configurations assuming that slow and rapid phase transitions occur at the sharp hadron–quark interface. We find that, unlike in the rapid transition scenario, where ∂M/∂²c &lt; 0 is a sufficient condition for instability, in the slow transition scenario there exists a connected extended stable branch beyond the maximum mass star, for which ∂M/∂²c &lt; 0. Finally, analysing the gravitational mass versus baryon mass relationship, we have calculated the energy released in transitions between stable stellar configurations. We find that the inclusion of the magnetic field and the existence of new stable branches allows the possibility of new channels of transitions that fulfil the energy requirements to explain gamma-ray bursts.Facultad de Ciencias Astronómicas y Geofísicas2019-09-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf4261-4277http://sedici.unlp.edu.ar/handle/10915/126594enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/issn/1365-2966info:eu-repo/semantics/altIdentifier/arxiv/1909.08661info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stz2392info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:29:53Zoai:sedici.unlp.edu.ar:10915/126594Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:29:53.612SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interface
title Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interface
spellingShingle Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interface
Mariani, Mauro
Ciencias Astronómicas
Dense matter
equation of state
stars: magnetars
stars: neutron
stars: oscillations
title_short Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interface
title_full Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interface
title_fullStr Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interface
title_full_unstemmed Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interface
title_sort Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interface
dc.creator.none.fl_str_mv Mariani, Mauro
Orsaria, Milva Gabriela
Ranea Sandoval, Ignacio Francisco
Lugones, Germán
author Mariani, Mauro
author_facet Mariani, Mauro
Orsaria, Milva Gabriela
Ranea Sandoval, Ignacio Francisco
Lugones, Germán
author_role author
author2 Orsaria, Milva Gabriela
Ranea Sandoval, Ignacio Francisco
Lugones, Germán
author2_role author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Dense matter
equation of state
stars: magnetars
stars: neutron
stars: oscillations
topic Ciencias Astronómicas
Dense matter
equation of state
stars: magnetars
stars: neutron
stars: oscillations
dc.description.none.fl_txt_mv We study the influence of strong magnetic fields in hybrid stars, composed by hadrons and a pure quark matter core, and analyse their structure and stability as well as some possible evolution channels due to the magnetic field decay. Using an ad hoc parametrization of the magnetic field strength and taking into account Landau-quantization effects in matter, we calculate hybrid magnetized equations of state and some associated quantities, such as particle abundances and matter magnetization, for different sets of parameters and different magnetic field strengths. Moreover, we compute the magnetized stable stellar configurations, the mass versus radius and the gravitational mass versus central energy density relationships, the gravitational mass versus baryon mass diagram, and the tidal deformability. Our results are in agreement with both, the∼ 2 M¯ pulsars and the data obtained from GW170817. In addition, we study the stability of stellar configurations assuming that slow and rapid phase transitions occur at the sharp hadron–quark interface. We find that, unlike in the rapid transition scenario, where ∂M/∂²c &lt; 0 is a sufficient condition for instability, in the slow transition scenario there exists a connected extended stable branch beyond the maximum mass star, for which ∂M/∂²c &lt; 0. Finally, analysing the gravitational mass versus baryon mass relationship, we have calculated the energy released in transitions between stable stellar configurations. We find that the inclusion of the magnetic field and the existence of new stable branches allows the possibility of new channels of transitions that fulfil the energy requirements to explain gamma-ray bursts.
Facultad de Ciencias Astronómicas y Geofísicas
description We study the influence of strong magnetic fields in hybrid stars, composed by hadrons and a pure quark matter core, and analyse their structure and stability as well as some possible evolution channels due to the magnetic field decay. Using an ad hoc parametrization of the magnetic field strength and taking into account Landau-quantization effects in matter, we calculate hybrid magnetized equations of state and some associated quantities, such as particle abundances and matter magnetization, for different sets of parameters and different magnetic field strengths. Moreover, we compute the magnetized stable stellar configurations, the mass versus radius and the gravitational mass versus central energy density relationships, the gravitational mass versus baryon mass diagram, and the tidal deformability. Our results are in agreement with both, the∼ 2 M¯ pulsars and the data obtained from GW170817. In addition, we study the stability of stellar configurations assuming that slow and rapid phase transitions occur at the sharp hadron–quark interface. We find that, unlike in the rapid transition scenario, where ∂M/∂²c &lt; 0 is a sufficient condition for instability, in the slow transition scenario there exists a connected extended stable branch beyond the maximum mass star, for which ∂M/∂²c &lt; 0. Finally, analysing the gravitational mass versus baryon mass relationship, we have calculated the energy released in transitions between stable stellar configurations. We find that the inclusion of the magnetic field and the existence of new stable branches allows the possibility of new channels of transitions that fulfil the energy requirements to explain gamma-ray bursts.
publishDate 2019
dc.date.none.fl_str_mv 2019-09-02
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/10915/126594
url http://sedici.unlp.edu.ar/handle/10915/126594
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0035-8711
info:eu-repo/semantics/altIdentifier/issn/1365-2966
info:eu-repo/semantics/altIdentifier/arxiv/1909.08661
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stz2392
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
4261-4277
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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