PAPPAS, Thomas, Nelson Camilo POSADA AGUIRRE and Zdeněk STUCHLÍK. Extended Tolman III and VII solutions in f (R, T) gravity: Models for neutron stars and supermassive stars. Physical Review D. 2022, vol. 106, No 12, p. "124014-1"-"124014-25", 25 pp. ISSN 2470-0010. Available from: https://dx.doi.org/10.1103/PhysRevD.106.124014.
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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
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher United States of America
Confidentiality degree is not subject to a state or trade secret
WWW URL
RIV identification code RIV/47813059:19630/22:A0000204
Organization unit Institute of physics in Opava
Doi http://dx.doi.org/10.1103/PhysRevD.106.124014
UT WoS 000901634800001
Keywords in English energy-momentum tensor;dimensionless parameter;numerical solution;isotropic perfect-fluid spheres
Tags FÚ, RIV23
Tags International impact, Reviewed
Changed by Changed by: Mgr. Pavlína Jalůvková, učo 25213. Changed: 7/3/2023 13:56.
Abstract
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.
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