Realistic neutron star models in f(T) gravity

• Published in: The 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
• Language: English
• 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
• ISSN: 1434-6052; 1434-6044; 1434-6052
• DOI: 10.1140/epjc/s10052-022-10268-2

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.