Rapidly rotating neutron stars in f (R, T) = R + 2λT gravity

被引：0

作者：

da Silva, F. M. ^{[1
]}

Santos, L. C. N. ^{[2
]}

Mota, C. E. ^{[3
]}

da Costa, T. O. F. ^{[1
]}

Fabris, J. C. ^{[1
,4
]}

机构：

[1] Univ Fed Espirito Santo, Dept Fis, Nucleo Cosmo Ufes, Av Fernando Ferrari,540, BR-29075910 Vitoria, ES, Brazil

[2] Univ Fed Paraiba, Dept Fis, CCEN, CP 5008, BR-58051970 Joao Pessoa, PB, Brazil

[3] Univ Fed Santa Catarina, Dept Fis, CFM, CP 476, BR-88040900 Florianopolis, SC, Brazil

[4] Natl Res Nucl Univ MEPhI, Kashirskoe sh 31, Moscow 115409, Russia

来源：

EUROPEAN PHYSICAL JOURNAL C | 2023年 / 83卷 / 04期

关键词：

EQUATION-OF-STATE; GENERAL RELATIVISTIC STARS; COVARIANT CONSERVATION; NUCLEAR-MATTER; STRANGE STARS; GRAVITY; ENERGY; MOMENTUM; INERTIA; HISTORY;

D O I：

10.1140/epjc/s10052-023-11466-2

中图分类号：

O412 [相对论、场论]; O572.2 [粒子物理学];

学科分类号：

摘要：

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.

引用

页数：14

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