Realistic neutron star models in f(T) gravity

We investigate the nonrotating neutron stars in f ( T ) gravity with f ( T ) = T + α T 2 , where T is the torsion scalar in the teleparallel formalism of gravity. In particular, we utilize the SLy and BSk family of equations of state for perfect fluid to describe the neutron stellar matter and searc...

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Published inThe European physical journal. C, Particles and fields Vol. 82; no. 4; pp. 1 - 16
Main Authors Lin, Rui-Hui, Chen, Xiao-Ning, Zhai, Xiang-Hua
Format Journal Article
LanguageEnglish
Published Berlin/Heidelberg Springer Berlin Heidelberg 01.04.2022
Springer
Springer Nature B.V
SpringerOpen
Subjects
Analysis
Astronomy
Astrophysics and Cosmology
Density
Elementary Particles
Equations of state
Gravitational waves
Hadrons
Heavy Ions
Mathematical models
Measurement Science and Instrumentation
Neutron stars
Neutrons
Nuclear Energy
Nuclear Physics
Phase transitions
Physics
Physics and Astronomy
Pulsars
Quantum Field Theories
Quantum Field Theory
Regular Article - Theoretical Physics
Relativity
Stellar mass
String Theory
Online AccessGet full text
ISSN1434-6052
1434-6044
1434-6052
DOI10.1140/epjc/s10052-022-10268-2

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Abstract We investigate the nonrotating neutron stars in f ( T ) gravity with f ( T ) = T + α T 2 , where T is the torsion scalar in the teleparallel formalism of gravity. In particular, we utilize the SLy and BSk family of equations of state for perfect fluid to describe the neutron stellar matter and search for the effects of the f ( T ) modification on the models of neutron stars. For positive α , the modification results in a smaller stellar mass in comparison to general relativity, while the neutron stars will contain larger amount of matter for negative α . Moreover, there seems to be an upper limit for the central density of the neutron stars with α > 0 , beyond which the effective f ( T ) fluid would have a steplike phase transition in density and pressure profiles, collapsing the numerical system. We obtain the mass–radius relations of the realistic models of neutron stars and subject them to the joint constraints from the observed massive pulsars PSR J0030+0451, PSR J0740+6620, and PSR J2215+5135, and gravitational wave events GW170817 and GW190814. For the neutron star model in f ( T ) gravity to be able to accommodate all the mentioned data, the model parameter α needs to be smaller than - 4.295 , - 6.476 , - 4.4 , and - 2.12 (in the unit of G 2 M ⊙ 2 / c 4 ) for SLy, BSk19, BSk20, and BSk21 equations of state, respectively. If one considers the unknown compact object in the event GW190814 not to be a neutron star and hence excludes this dataset, the constraints can be loosened to α < - 0.594 , - 3.5 , 0.4 and 1.9 (in the unit of G 2 M ⊙ 2 / c 4 ), respectively.
AbstractList We investigate the nonrotating neutron stars in f(T) gravity with f(T)=T+αT2, where T is the torsion scalar in the teleparallel formalism of gravity. In particular, we utilize the SLy and BSk family of equations of state for perfect fluid to describe the neutron stellar matter and search for the effects of the f(T) modification on the models of neutron stars. For positive α, the modification results in a smaller stellar mass in comparison to general relativity, while the neutron stars will contain larger amount of matter for negative α. Moreover, there seems to be an upper limit for the central density of the neutron stars with α>0, beyond which the effective f(T) fluid would have a steplike phase transition in density and pressure profiles, collapsing the numerical system. We obtain the mass–radius relations of the realistic models of neutron stars and subject them to the joint constraints from the observed massive pulsars PSR J0030+0451, PSR J0740+6620, and PSR J2215+5135, and gravitational wave events GW170817 and GW190814. For the neutron star model in f(T) gravity to be able to accommodate all the mentioned data, the model parameter α needs to be smaller than -4.295, -6.476, -4.4, and -2.12 (in the unit of G2M⊙2/c4) for SLy, BSk19, BSk20, and BSk21 equations of state, respectively. If one considers the unknown compact object in the event GW190814 not to be a neutron star and hence excludes this dataset, the constraints can be loosened to α<-0.594, -3.5, 0.4 and 1.9 (in the unit of G2M⊙2/c4), respectively.
We investigate the nonrotating neutron stars in f ( T ) gravity with f ( T ) = T + α T 2 , where T is the torsion scalar in the teleparallel formalism of gravity. In particular, we utilize the SLy and BSk family of equations of state for perfect fluid to describe the neutron stellar matter and search for the effects of the f ( T ) modification on the models of neutron stars. For positive α , the modification results in a smaller stellar mass in comparison to general relativity, while the neutron stars will contain larger amount of matter for negative α . Moreover, there seems to be an upper limit for the central density of the neutron stars with α > 0 , beyond which the effective f ( T ) fluid would have a steplike phase transition in density and pressure profiles, collapsing the numerical system. We obtain the mass–radius relations of the realistic models of neutron stars and subject them to the joint constraints from the observed massive pulsars PSR J0030+0451, PSR J0740+6620, and PSR J2215+5135, and gravitational wave events GW170817 and GW190814. For the neutron star model in f ( T ) gravity to be able to accommodate all the mentioned data, the model parameter α needs to be smaller than - 4.295 , - 6.476 , - 4.4 , and - 2.12 (in the unit of G 2 M ⊙ 2 / c 4 ) for SLy, BSk19, BSk20, and BSk21 equations of state, respectively. If one considers the unknown compact object in the event GW190814 not to be a neutron star and hence excludes this dataset, the constraints can be loosened to α < - 0.594 , - 3.5 , 0.4 and 1.9 (in the unit of G 2 M ⊙ 2 / c 4 ), respectively.
Abstract We investigate the nonrotating neutron stars in f(T) gravity with $$f(T)=T+\alpha {T}^2$$ f ( T ) = T + α T 2 , where T is the torsion scalar in the teleparallel formalism of gravity. In particular, we utilize the SLy and BSk family of equations of state for perfect fluid to describe the neutron stellar matter and search for the effects of the f(T) modification on the models of neutron stars. For positive $$\alpha $$ α , the modification results in a smaller stellar mass in comparison to general relativity, while the neutron stars will contain larger amount of matter for negative $$\alpha $$ α . Moreover, there seems to be an upper limit for the central density of the neutron stars with $$\alpha >0$$ α > 0 , beyond which the effective f(T) fluid would have a steplike phase transition in density and pressure profiles, collapsing the numerical system. We obtain the mass–radius relations of the realistic models of neutron stars and subject them to the joint constraints from the observed massive pulsars PSR J0030+0451, PSR J0740+6620, and PSR J2215+5135, and gravitational wave events GW170817 and GW190814. For the neutron star model in f(T) gravity to be able to accommodate all the mentioned data, the model parameter $$\alpha $$ α needs to be smaller than $$-\,4.295$$ - 4.295 , $$-\,6.476$$ - 6.476 , $$-\,4.4$$ - 4.4 , and $$-\,2.12$$ - 2.12 (in the unit of $${G}^2M_\odot ^2/c^4$$ G 2 M ⊙ 2 / c 4 ) for SLy, BSk19, BSk20, and BSk21 equations of state, respectively. If one considers the unknown compact object in the event GW190814 not to be a neutron star and hence excludes this dataset, the constraints can be loosened to $$\alpha <-\,0.594$$ α < - 0.594 , $$-\,3.5$$ - 3.5 , 0.4 and 1.9 (in the unit of $${G}^2M_\odot ^2/c^4$$ G 2 M ⊙ 2 / c 4 ), respectively.
We investigate the nonrotating neutron stars in f ( T ) gravity with $$f(T)=T+\alpha {T}^2$$ f ( T ) = T + α T 2 , where T is the torsion scalar in the teleparallel formalism of gravity. In particular, we utilize the SLy and BSk family of equations of state for perfect fluid to describe the neutron stellar matter and search for the effects of the f ( T ) modification on the models of neutron stars. For positive $$\alpha $$ α , the modification results in a smaller stellar mass in comparison to general relativity, while the neutron stars will contain larger amount of matter for negative $$\alpha $$ α . Moreover, there seems to be an upper limit for the central density of the neutron stars with $$\alpha >0$$ α > 0 , beyond which the effective f ( T ) fluid would have a steplike phase transition in density and pressure profiles, collapsing the numerical system. We obtain the mass–radius relations of the realistic models of neutron stars and subject them to the joint constraints from the observed massive pulsars PSR J0030+0451, PSR J0740+6620, and PSR J2215+5135, and gravitational wave events GW170817 and GW190814. For the neutron star model in f ( T ) gravity to be able to accommodate all the mentioned data, the model parameter $$\alpha $$ α needs to be smaller than $$-\,4.295$$ - 4.295 , $$-\,6.476$$ - 6.476 , $$-\,4.4$$ - 4.4 , and $$-\,2.12$$ - 2.12 (in the unit of $${G}^2M_\odot ^2/c^4$$ G 2 M ⊙ 2 / c 4 ) for SLy, BSk19, BSk20, and BSk21 equations of state, respectively. If one considers the unknown compact object in the event GW190814 not to be a neutron star and hence excludes this dataset, the constraints can be loosened to $$\alpha <-\,0.594$$ α < - 0.594 , $$-\,3.5$$ - 3.5 , 0.4 and 1.9 (in the unit of $${G}^2M_\odot ^2/c^4$$ G 2 M ⊙ 2 / c 4 ), respectively.
We investigate the nonrotating neutron stars in f(T) gravity with [Formula omitted], where T is the torsion scalar in the teleparallel formalism of gravity. In particular, we utilize the SLy and BSk family of equations of state for perfect fluid to describe the neutron stellar matter and search for the effects of the f(T) modification on the models of neutron stars. For positive [Formula omitted], the modification results in a smaller stellar mass in comparison to general relativity, while the neutron stars will contain larger amount of matter for negative [Formula omitted]. Moreover, there seems to be an upper limit for the central density of the neutron stars with [Formula omitted], beyond which the effective f(T) fluid would have a steplike phase transition in density and pressure profiles, collapsing the numerical system. We obtain the mass-radius relations of the realistic models of neutron stars and subject them to the joint constraints from the observed massive pulsars PSR J0030+0451, PSR J0740+6620, and PSR J2215+5135, and gravitational wave events GW170817 and GW190814. For the neutron star model in f(T) gravity to be able to accommodate all the mentioned data, the model parameter [Formula omitted] needs to be smaller than [Formula omitted], [Formula omitted], [Formula omitted], and [Formula omitted] (in the unit of [Formula omitted]) for SLy, BSk19, BSk20, and BSk21 equations of state, respectively. If one considers the unknown compact object in the event GW190814 not to be a neutron star and hence excludes this dataset, the constraints can be loosened to [Formula omitted], [Formula omitted], 0.4 and 1.9 (in the unit of [Formula omitted]), respectively.
ArticleNumber 308
Audience Academic
Author Lin, Rui-Hui
Chen, Xiao-Ning
Zhai, Xiang-Hua
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  surname: Zhai
  fullname: Zhai, Xiang-Hua
  email: zhaixh@shnu.edu.cn
  organization: Division of Mathematics and Theoretical Physics, Shanghai Normal University
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Snippet We investigate the nonrotating neutron stars in f ( T ) gravity with f ( T ) = T + α T 2 , where T is the torsion scalar in the teleparallel formalism of...
We investigate the nonrotating neutron stars in f ( T ) gravity with $$f(T)=T+\alpha {T}^2$$ f ( T ) = T + α T 2 , where T is the torsion scalar in the...
We investigate the nonrotating neutron stars in f(T) gravity with [Formula omitted], where T is the torsion scalar in the teleparallel formalism of gravity. In...
We investigate the nonrotating neutron stars in f(T) gravity with f(T)=T+αT2, where T is the torsion scalar in the teleparallel formalism of gravity. In...
Abstract We investigate the nonrotating neutron stars in f(T) gravity with $$f(T)=T+\alpha {T}^2$$ f ( T ) = T + α T 2 , where T is the torsion scalar in the...
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SubjectTerms Analysis
Astronomy
Astrophysics and Cosmology
Density
Elementary Particles
Equations of state
Gravitational waves
Hadrons
Heavy Ions
Mathematical models
Measurement Science and Instrumentation
Neutron stars
Neutrons
Nuclear Energy
Nuclear Physics
Phase transitions
Physics
Physics and Astronomy
Pulsars
Quantum Field Theories
Quantum Field Theory
Regular Article - Theoretical Physics
Relativity
Stellar mass
String Theory
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Title Realistic neutron star models in f(T) gravity
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