Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology

Descripción del Articulo

El texto completo de este trabajo no está disponible en el Repositorio Académico UPN por restricciones de la casa editorial donde ha sido publicado.
Detalles Bibliográficos
Autores: Pretel, Juan M. Z., Jorás, Sergio E., Reis, Ribamar R. R., Arbañil, José D. V.
Formato: artículo
Fecha de Publicación:2021
Institución:Universidad Privada del Norte
Repositorio:UPN-Institucional
Lenguaje:inglés
OAI Identifier:oai:repositorio.upn.edu.pe:11537/28467
Enlace del recurso:https://hdl.handle.net/11537/28467
https://doi.org/10.1088/1475-7516/2021/08/055
Nivel de acceso:acceso cerrado
Materia:Estrellas
Energía
Gravedad
https://purl.org/pe-repo/ocde/ford#2.07.00
id UUPN_0dc8f0da251d74ecb6eb27363d163935
oai_identifier_str oai:repositorio.upn.edu.pe:11537/28467
network_acronym_str UUPN
network_name_str UPN-Institucional
repository_id_str 1873
dc.title.es_PE.fl_str_mv Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology
title Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology
spellingShingle Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology
Pretel, Juan M. Z.
Estrellas
Energía
Gravedad
https://purl.org/pe-repo/ocde/ford#2.07.00
title_short Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology
title_full Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology
title_fullStr Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology
title_full_unstemmed Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology
title_sort Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology
author Pretel, Juan M. Z.
author_facet Pretel, Juan M. Z.
Jorás, Sergio E.
Reis, Ribamar R. R.
Arbañil, José D. V.
author_role author
author2 Jorás, Sergio E.
Reis, Ribamar R. R.
Arbañil, José D. V.
author2_role author
author
author
dc.contributor.author.fl_str_mv Pretel, Juan M. Z.
Jorás, Sergio E.
Reis, Ribamar R. R.
Arbañil, José D. V.
dc.subject.es_PE.fl_str_mv Estrellas
Energía
Gravedad
topic Estrellas
Energía
Gravedad
https://purl.org/pe-repo/ocde/ford#2.07.00
dc.subject.ocde.es_PE.fl_str_mv https://purl.org/pe-repo/ocde/ford#2.07.00
description El texto completo de este trabajo no está disponible en el Repositorio Académico UPN por restricciones de la casa editorial donde ha sido publicado.
publishDate 2021
dc.date.accessioned.none.fl_str_mv 2021-11-18T06:11:31Z
dc.date.available.none.fl_str_mv 2021-11-18T06:11:31Z
dc.date.issued.fl_str_mv 2021-08-24
dc.type.es_PE.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.citation.es_PE.fl_str_mv Pretel, J. M., ...[et al.]. (2021). Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology. Journal Of Cosmology And Astroparticle Physics, 8(55). https://doi.org/10.1088/1475-7516/2021/08/055
dc.identifier.uri.none.fl_str_mv https://hdl.handle.net/11537/28467
dc.identifier.journal.es_PE.fl_str_mv Journal Of Cosmology And Astroparticle Physics
dc.identifier.doi.none.fl_str_mv https://doi.org/10.1088/1475-7516/2021/08/055
identifier_str_mv Pretel, J. M., ...[et al.]. (2021). Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology. Journal Of Cosmology And Astroparticle Physics, 8(55). https://doi.org/10.1088/1475-7516/2021/08/055
Journal Of Cosmology And Astroparticle Physics
url https://hdl.handle.net/11537/28467
https://doi.org/10.1088/1475-7516/2021/08/055
dc.language.iso.es_PE.fl_str_mv eng
language eng
dc.rights.es_PE.fl_str_mv info:eu-repo/semantics/closedAccess
eu_rights_str_mv closedAccess
dc.format.es_PE.fl_str_mv application/pdf
dc.publisher.es_PE.fl_str_mv IOP Publishing
dc.publisher.country.es_PE.fl_str_mv GB
dc.source.es_PE.fl_str_mv Universidad Privada del Norte
Repositorio Institucional - UPN
dc.source.none.fl_str_mv reponame:UPN-Institucional
instname:Universidad Privada del Norte
instacron:UPN
instname_str Universidad Privada del Norte
instacron_str UPN
institution UPN
reponame_str UPN-Institucional
collection UPN-Institucional
bitstream.url.fl_str_mv https://repositorio.upn.edu.pe/bitstream/11537/28467/1/license.txt
bitstream.checksum.fl_str_mv 8a4605be74aa9ea9d79846c1fba20a33
bitstream.checksumAlgorithm.fl_str_mv MD5
repository.name.fl_str_mv Repositorio Institucional UPN
repository.mail.fl_str_mv jordan.rivero@upn.edu.pe
_version_ 1752944258967404544
spelling Pretel, Juan M. Z.Jorás, Sergio E.Reis, Ribamar R. R.Arbañil, José D. V.2021-11-18T06:11:31Z2021-11-18T06:11:31Z2021-08-24Pretel, J. M., ...[et al.]. (2021). Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology. Journal Of Cosmology And Astroparticle Physics, 8(55). https://doi.org/10.1088/1475-7516/2021/08/055https://hdl.handle.net/11537/28467Journal Of Cosmology And Astroparticle Physicshttps://doi.org/10.1088/1475-7516/2021/08/055El texto completo de este trabajo no está disponible en el Repositorio Académico UPN por restricciones de la casa editorial donde ha sido publicado.ABSTRACT We investigate the equilibrium and radial stability of spherically symmetric relativistic stars, considering a polytropic equation of state (EoS), within the framework of f(R,T) gravity with a conservative energy-momentum tensor. Both modified stellar structure equations and Chandrasekhar's pulsation equations are derived for the f(R,T)= R+ h(T) gravity model, where the function h(T) assumes a specific form in order to safeguard the conservation equation for the energy-momentum tensor. The neutron star properties, such as radius, mass, binding energy and oscillation spectrum are studied in detail. Our results show that a cusp — which signals the appearance of instability — is formed when the binding energy is plotted as a function of the compact star proper mass. We find that the squared frequency of the fundamental vibration mode passes through zero at the central-density value corresponding to such a cusp where the binding energy is a minimum.Revisión por paresSan Juan de Luriganchoapplication/pdfengIOP PublishingGBinfo:eu-repo/semantics/closedAccessUniversidad Privada del NorteRepositorio Institucional - UPNreponame:UPN-Institucionalinstname:Universidad Privada del Norteinstacron:UPNEstrellasEnergíaGravedadhttps://purl.org/pe-repo/ocde/ford#2.07.00Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismologyinfo:eu-repo/semantics/articleLICENSElicense.txtlicense.txttext/plain; charset=utf-81748https://repositorio.upn.edu.pe/bitstream/11537/28467/1/license.txt8a4605be74aa9ea9d79846c1fba20a33MD5111537/28467oai:repositorio.upn.edu.pe:11537/284672021-11-18 01:11:37.016Repositorio Institucional UPNjordan.rivero@upn.edu.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
score 13.888049
Neutron stars in f(R,T) gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology
Nota importante:
La información contenida en este registro es de entera responsabilidad de la institución que gestiona el repositorio institucional donde esta contenido este documento o set de datos. El CONCYTEC no se hace responsable por los contenidos (publicaciones y/o datos) accesibles a través del Repositorio Nacional Digital de Ciencia, Tecnología e Innovación de Acceso Abierto (ALICIA).

Ejemplares Similares