Rotating neutron stars in F(R) gravity with axions

We investigate equilibrium configurations of uniformly rotating neutron stars in R2 gravity with axion scalar field for GM1 equation of state (EoS) for nuclear matter. The mass-radius diagram, mass-central energy density are presented for some frequencies in comparison with static stars. We also com...

Full description

Bibliographic Details
Authors: Astashenok, Artyom V., Odintsov, Sergei D.
Format: article
Status:Published version
Publication Date:2020
Country:España
Institution:Consejo Superior de Investigaciones Científicas (CSIC)
Repository:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/237276
Online Access:http://hdl.handle.net/10261/237276
Access Level:Open access
Keyword:Dark matter
Stars: neutron
Stars: rotation
id ES_dd4ecb3c9e5ec6eb436eecaf2a30d987
oai_identifier_str oai:digital.csic.es:10261/237276
network_acronym_str ES
network_name_str España
repository_id_str
spelling Rotating neutron stars in F(R) gravity with axionsAstashenok, Artyom V.Odintsov, Sergei D.Dark matterStars: neutronStars: rotationWe investigate equilibrium configurations of uniformly rotating neutron stars in R2 gravity with axion scalar field for GM1 equation of state (EoS) for nuclear matter. The mass-radius diagram, mass-central energy density are presented for some frequencies in comparison with static stars. We also compute equatorial and polar radii and moment of inertia for stars. For axion field φ, the coupling in the form ∼R2φ is assumed. Several interesting results follow from our consideration. Maximal possible star mass with given EoS increases due to the contribution of coupling term. We discovered the possibility to increase maximal frequency of the rotation in comparison with General Relativity. As a consequence, the lower bound on mass of the fast rotating stars decreases. For frequency f = 700 Hz, neutron stars with masses ∼M⊙ can exist for some choice of parameters (in General Relativity for same EoS, this limit is around 1.2 M⊙). Another feature of our solutions is relatively small increase of stars' radii for high frequencies in comparison with static case. Thus, eventually, the new class of neutron stars in R2 gravity with axions is discovered namely fast rotating compact stars with intermediate masses.Royal Astronomical SocietyConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2021202120202021info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/237276reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Ingléshttp://doi.org/10.1093/mnras/staa2630Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2372762026-05-22T06:33:51Z
dc.title.none.fl_str_mv Rotating neutron stars in F(R) gravity with axions
title Rotating neutron stars in F(R) gravity with axions
spellingShingle Rotating neutron stars in F(R) gravity with axions
Astashenok, Artyom V.
Dark matter
Stars: neutron
Stars: rotation
title_short Rotating neutron stars in F(R) gravity with axions
title_full Rotating neutron stars in F(R) gravity with axions
title_fullStr Rotating neutron stars in F(R) gravity with axions
title_full_unstemmed Rotating neutron stars in F(R) gravity with axions
title_sort Rotating neutron stars in F(R) gravity with axions
dc.creator.none.fl_str_mv Astashenok, Artyom V.
Odintsov, Sergei D.
author Astashenok, Artyom V.
author_facet Astashenok, Artyom V.
Odintsov, Sergei D.
author_role author
author2 Odintsov, Sergei D.
author2_role author
dc.contributor.none.fl_str_mv Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Dark matter
Stars: neutron
Stars: rotation
topic Dark matter
Stars: neutron
Stars: rotation
description We investigate equilibrium configurations of uniformly rotating neutron stars in R2 gravity with axion scalar field for GM1 equation of state (EoS) for nuclear matter. The mass-radius diagram, mass-central energy density are presented for some frequencies in comparison with static stars. We also compute equatorial and polar radii and moment of inertia for stars. For axion field φ, the coupling in the form ∼R2φ is assumed. Several interesting results follow from our consideration. Maximal possible star mass with given EoS increases due to the contribution of coupling term. We discovered the possibility to increase maximal frequency of the rotation in comparison with General Relativity. As a consequence, the lower bound on mass of the fast rotating stars decreases. For frequency f = 700 Hz, neutron stars with masses ∼M⊙ can exist for some choice of parameters (in General Relativity for same EoS, this limit is around 1.2 M⊙). Another feature of our solutions is relatively small increase of stars' radii for high frequencies in comparison with static case. Thus, eventually, the new class of neutron stars in R2 gravity with axions is discovered namely fast rotating compact stars with intermediate masses.
publishDate 2020
dc.date.none.fl_str_mv 2020
2021
2021
2021
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/10261/237276
url http://hdl.handle.net/10261/237276
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv http://doi.org/10.1093/mnras/staa2630
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv Royal Astronomical Society
publisher.none.fl_str_mv Royal Astronomical Society
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
_version_ 1869421848807079936
score 15,812429

Similar Items