J 2022

Extended Tolman III and VII solutions in f (R, T) gravity: Models for neutron stars and supermassive stars

PAPPAS, Thomas, Nelson Camilo POSADA AGUIRRE and Zdeněk STUCHLÍK

Basic information

Original name

Extended Tolman III and VII solutions in f (R, T) gravity: Models for neutron stars and supermassive stars

Authors

PAPPAS, Thomas (300 Greece, belonging to the institution), Nelson Camilo POSADA AGUIRRE (170 Colombia, belonging to the institution) and Zdeněk STUCHLÍK (203 Czech Republic, belonging to the institution)

Edition

Physical Review D, 2022, 2470-0010

Other information

Language

English

Type of outcome

Článek v odborném periodiku

Field of Study

10308 Astronomy

Country of publisher

United States of America

Confidentiality degree

není předmětem státního či obchodního tajemství

References:

RIV identification code

RIV/47813059:19630/22:A0000204

Organization unit

Institute of physics in Opava

UT WoS

000901634800001

Keywords in English

energy-momentum tensor;dimensionless parameter;numerical solution;isotropic perfect-fluid spheres

Tags

Tags

International impact, Reviewed
Změněno: 7/3/2023 13:56, Mgr. Pavlína Jalůvková

Abstract

V originále

In the context of linear f(R, T) = R chi T gravity, where R is the Ricci scalar, T is the trace of the energy-momentum tensor, and chi is a dimensionless parameter, we have obtained exact analytical and numerical solutions for isotropic perfect-fluid spheres in hydrostatic equilibrium. Our solutions correspond to two-parametric extensions of the Tolman III (T-III) and Tolman VII (T-VII) models, in terms of the compactness beta and chi. By requiring configurations that exhibit monotonically decreasing radial profiles for both the energy density and pressure, compliance with the energy conditions, as well as subluminal speed of sound, we have constrained the parametric space of our solutions. We have also obtained analytically a parametric deformation of the T-VII solution that continuously interpolates between the T-III and T-VII models for any chi, and in the appropriate limits, provides an analytic approximation for the uniform density configuration in linear f(R, T) gravity. Finally, by integrating numerically the TOV equations, we have obtained a numerical solution for the uniform-density configuration and subsequently, using the mass -radius relations, we have obtained the maximum mass that can be supported by such configurations. We have found that in the appropriate parametric regime our solution is in very good agreement with the observational bounds for the masses and radii of neutron stars.