Hydrostatic equilibrium configurations of neutron stars in the f (R, L, T) gravity theory

被引：0

作者：

Fortunato, J. A. S. ^{[1
]}

Moraes, P. H. R. S. ^{[2
]}

Brito, E. ^{[3
]}

de Lima Junior, J. G. ^{[4
]}

Guerini, T. S. ^{[5
]}

机构：

[1] Univ Fed Espirito Santo UFES, PPGCosmo, CCE, Av Fernando Ferrari 540, Vitoria BR-29075910, ES, Brazil

[2] Univ Cidade Sao Paulo UNICID, Lab Fis Teor & Computac LFTC, Rua Galvao Bueno 868, Sao Paulo, SP, Brazil

[3] Univ Fed Oeste Bahia, Ctr Ciencias Exatas & Tecnol, Rua Bertioga 892, BR-47810059 Barreiras, BA, Brazil

[4] Univ Fed Alagoas UFAL, Inst Fis, Ave Lourival Melo Mota, BR-57072970 Maceio, AL, Brazil

[5] Univ Estado Rio de Janeiro UERJ, Inst Fis, Rua Sao Francisco Xavier 524, BR-20550013 Rio De Janeiro, RJ, Brazil

来源：

PHYSICS OF THE DARK UNIVERSE | 2025年 / 48卷

关键词：

Modified gravity; Neutron stars; TOV equation; Equations of state; F(R) THEORIES; EQUATIONS; MASS;

D O I：

10.1016/j.dark.2025.101893

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In the present work, we obtain the hydrostatic equilibrium configurations of neutron stars in the recently proposed f(R,L,T) theory of gravity, for which R is the Ricci scalar, L is the matter lagrangian density, T is the trace of the energy-momentum tensor and f is a function of the argument. This theory emerges in the present literature as a generalized geometry-matter coupling theory of gravity. We derive the Tolman-Oppenheimer-Volkoff-like equation for a particular functional form of the f(R,L,T) function. Our solutions are obtained from realistic equations of state describing matter inside neutron stars. We obtain stable solutions for neutron stars and we show that for some values of the free parameter of the theory it is possible to be in agreement with both NICER and LIGO/Virgo observational data. We also calculate the surface gravitational redshift for the f (R, L, T) gravity neutron stars.

引用

页数：7