Regular Article - Theoretical Physics
Rapidly rotating neutron stars in gravity
Núcleo Cosmo-ufes, Departamento de Física, Universidade Federal do Espírito Santo, Av. Fernando Ferrari, 540, CEP 29.075-910, Vitória, ES, Brazil
2 Departamento de Física, CCEN-Universidade Federal da Paraíba, C.P. 5008, CEP 58.051-970, João Pessoa, PB, Brazil
3 Departamento de Física, CFM-Universidade Federal de Santa Catarina, C.P. 476, CEP 88.040-900, Florianópolis, SC, Brazil
4 National Research Nuclear University MEPhI, Kashirskoe sh.31, 115409, Moscow, Russia
Accepted: 2 April 2023
Published online: 14 April 2023
In this work, we study the influence of f(R, T) gravity on rapidly rotating neutron stars. First we discuss the main aspects of this modified theory of gravity where the gravitational Lagrangian is an arbitrary function of the Ricci scalar R and of the trace of the energy–momentum tensor T. Then we present the basic equations for neutron stars including the equations of state used in the present work to describe the hadronic matter. Some physical quantities of interest are calculated such as mass–radius relations, moments of inertia, angular momentum, and compactness. By considering four different rotation regimes, we obtain results that indicate substantial modifications in the physical properties of neutron stars in f(R, T) gravity when compared to those in the context of general relativity. In particular, the mass–radius relation for sequences of stars indicates that f(R, T) gravity increases the mass and the equatorial radius of the neutron stars for stars rotating with an angular velocity smaller than Kepler limit.
© The Author(s) 2023
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