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∼ 2M 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/∂c < 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/∂c < 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.
Fil: Mariani, Mauro. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina
Fil: Orsaria, Milva Gabriela. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Ranea Sandoval, Ignacio Francisco. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Lugones, Germán. Universidad Federal Do Abc; Brasil
Materia
DENSE MATTER
EQUATION OF STATE
STARS: MAGNETARS
STARS: NEUTRON
STARS: OSCILLATIONS
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/128435
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/128435
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interfaceMariani, MauroOrsaria, Milva GabrielaRanea Sandoval, Ignacio FranciscoLugones, GermánDENSE MATTEREQUATION OF STATESTARS: MAGNETARSSTARS: NEUTRONSTARS: OSCILLATIONShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We 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∼ 2M 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/∂c < 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/∂c < 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.Fil: Mariani, Mauro. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; ArgentinaFil: Orsaria, Milva Gabriela. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Ranea Sandoval, Ignacio Francisco. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Lugones, Germán. Universidad Federal Do Abc; BrasilWiley Blackwell Publishing, Inc2019-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/128435Mariani, Mauro; Orsaria, Milva Gabriela; Ranea Sandoval, Ignacio Francisco; Lugones, Germán; Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interface; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 489; 3; 11-2019; 4261-42770035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stz2392/5558243info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stz2392info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T12:09:48Zoai:ri.conicet.gov.ar:11336/128435instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-22 12:09:48.898CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
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
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 DENSE MATTER
EQUATION OF STATE
STARS: MAGNETARS
STARS: NEUTRON
STARS: OSCILLATIONS
topic DENSE MATTER
EQUATION OF STATE
STARS: MAGNETARS
STARS: NEUTRON
STARS: OSCILLATIONS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
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∼ 2M 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/∂c < 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/∂c < 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.
Fil: Mariani, Mauro. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina
Fil: Orsaria, Milva Gabriela. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Ranea Sandoval, Ignacio Francisco. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Lugones, Germán. Universidad Federal Do Abc; Brasil
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∼ 2M 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/∂c < 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/∂c < 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 2019-11
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
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://hdl.handle.net/11336/128435
Mariani, Mauro; Orsaria, Milva Gabriela; Ranea Sandoval, Ignacio Francisco; Lugones, Germán; Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interface; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 489; 3; 11-2019; 4261-4277
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/128435
identifier_str_mv Mariani, Mauro; Orsaria, Milva Gabriela; Ranea Sandoval, Ignacio Francisco; Lugones, Germán; Magnetized hybrid stars: Effects of slow and rapid phase transitions at the quark-hadron interface; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 489; 3; 11-2019; 4261-4277
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stz2392/5558243
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stz2392
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 12.982451

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