Affiliation:
1. Centro Brasileiro de Pesquisas Físicas, Rua Dr. Xavier Sigaud, 150 URCA, Rio de Janeiro CEP 22290-180, RJ, Brazil
Abstract
Within the framework of [Formula: see text] theories of gravity, we investigate the hydrostatic equilibrium of anisotropic neutron stars with a physically relevant equation of state (EoS) for the radial pressure. In particular, we focus on the [Formula: see text] model, where [Formula: see text] is a minimal coupling constant. In the slowly rotating approximation, we derive the modified TOV equations and the expression for the relativistic moment of inertia. The main properties of neutron stars, such as radius, mass and moment of inertia, are studied in detail. Our results reveal that the main consequence of the [Formula: see text] term is a substantial increase in the surface radius for low enough central densities. Nevertheless, such a term slightly modifies the total gravitational mass and moment of inertia of the slowly rotating stars. Furthermore, the changes are noticeable when anisotropy is incorporated into the stellar fluid, and it is possible to obtain higher masses that are consistent with the current observational data.
Funder
Conselho Nacional de Desenvolvimento Científico e Tecnológico
Publisher
World Scientific Pub Co Pte Ltd
Subject
General Physics and Astronomy,Astronomy and Astrophysics,Nuclear and High Energy Physics
Cited by
22 articles.
订阅此论文施引文献
订阅此论文施引文献,注册后可以免费订阅5篇论文的施引文献,订阅后可以查看论文全部施引文献