Realistic neutron star models in f(T) gravity
Rui-Hui Lin, Xiaoning Chen, Xiang-Hua Zhai
Abstract
Abstract We investigate the nonrotating neutron stars in f ( T ) gravity with $$f(T)=T+\alpha {T}^2$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mi>f</mml:mi> <mml:mrow> <mml:mo>(</mml:mo> <mml:mi>T</mml:mi> <mml:mo>)</mml:mo> </mml:mrow> <mml:mo>=</mml:mo> <mml:mi>T</mml:mi> <mml:mo>+</mml:mo> <mml:mi>α</mml:mi> <mml:msup> <mml:mrow> <mml:mi>T</mml:mi> </mml:mrow> <mml:mn>2</mml:mn> </mml:msup> </mml:mrow> </mml:math> , 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 $$\alpha $$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>α</mml:mi> </mml:math> , 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 $$\alpha $$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>α</mml:mi> </mml:math> . Moreover, there seems to be an upper limit for the central density of the neutron stars with $$\alpha >0$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mi>α</mml:mi> <mml:mo>></mml:mo> <mml:mn>0</mml:mn> </mml:mrow> </mml:math> , 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 $$\alpha $$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>α</mml:mi> </mml:math> needs to be smaller than $$-\,4.295$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mo>-</mml:mo> <mml:mspace/> <mml:mn>4.295</mml:mn> </mml:mrow> </mml:math> , $$-\,6.476$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mo>-</mml:mo> <mml:mspace/> <mml:mn>6.476</mml:mn> </mml:mrow> </mml:math> , $$-\,4.4$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mo>-</mml:mo> <mml:mspace/> <mml:mn>4.4</mml:mn> </mml:mrow> </mml:math> , and $$-\,2.12$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mo>-</mml:mo> <mml:mspace/> <mml:mn>2.12</mml:mn> </mml:mrow> </mml:math> (in the unit of $${G}^2M_\odot ^2/c^4$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:msup> <mml:mrow> <mml:mi>G</mml:mi> </mml:mrow> <mml:mn>2</mml:mn> </mml:msup> <mml:msubsup> <mml:mi>M</mml:mi> <mml:mo>⊙</mml:mo> <mml:mn>2</mml:mn> </mml:msubsup> <mml:mo>/</mml:mo> <mml:msup> <mml:mi>c</mml:mi> <mml:mn>4</mml:mn> </mml:msup> </mml:mrow> </mml:math> ) 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 $$\alpha <-\,0.594$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mi>α</mml:mi> <mml:mo><</mml:mo> <mml:mo>-</mml:mo> <mml:mspace/> <mml:mn>0.594</mml:mn> </mml:mrow> </mml:math> , $$-\,3.5$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mo>-</mml:mo> <mml:mspace/> <mml:mn>3.5</mml:mn> </mml:mrow> </mml:math> , 0.4 and 1.9 (in the unit of $${G}^2M_\odot ^2/c^4$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:msup> <mml:mrow> <mml:mi>G</mml:mi> </mml:mrow> <mml:mn>2</mml:mn> </mml:msup> <mml:msubsup> <mml:mi>M</mml:mi> <mml:mo>⊙</mml:mo> <mml:mn>2</mml:mn> </mml:msubsup> <mml:mo>/</mml:mo> <mml:msup> <mml:mi>c</mml:mi> <mml:mn>4</mml:mn> </mml:msup> </mml:mrow> </mml:math> ), respectively.