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

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 . Th...

Full description

Saved in:
Bibliographic Details
Published in:The European physical journal. C, Particles and fields Particles and fields, 2023-04, Vol.83 (4), p.295, Article 295
Main Authors: da Silva, F. M., Santos, L. C. N., Mota, C. E., da Costa, T. O. F., Fabris, J. C.
Format: Article
Language:English
Subjects:
Angular momentum
Angular velocity
Astronomy
Astrophysics and Cosmology
Elementary Particles
Equations of state
Gravitation theory
Gravity
Hadrons
Heavy Ions
Mathematical analysis
Measurement Science and Instrumentation
Moments of inertia
Neutron stars
Neutrons
Nuclear Energy
Nuclear Physics
Physical properties
Physics
Physics and Astronomy
Quantum Field Theories
Quantum Field Theory
Regular Article - Theoretical Physics
Relativity
Stellar rotation
String Theory
Tensors
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary: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.
ISSN:1434-6052
1434-6044
1434-6052
DOI:10.1140/epjc/s10052-023-11466-2