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

@article{65731,
   author = {Pappas, Thomas and Posada Aguirre, Nelson Camilo and Stuchlík, Zdeněk},
   article_number = {12},
   doi = {http://dx.doi.org/10.1103/PhysRevD.106.124014},
   keywords = {energy-momentum tensor;dimensionless parameter;numerical solution;isotropic perfect-fluid spheres},
   language = {eng},
   issn = {2470-0010},
   journal = {Physical Review D},
   title = {Extended Tolman III and VII solutions in f (R, T) gravity: Models for neutron stars and supermassive stars},
   url = {https://journals.aps.org/prd/abstract/10.1103/PhysRevD.106.124014},
   volume = {106},
   year = {2022}
}

TY  - JOUR
ID  - 65731
AU  - Pappas, Thomas - Posada Aguirre, Nelson Camilo - Stuchlík, Zdeněk
PY  - 2022
TI  - Extended Tolman III and VII solutions in f (R, T) gravity: Models for neutron stars and supermassive stars
JF  - Physical Review D
VL  - 106
IS  - 12
SP  - "124014-1"-"124014-25"
EP  - "124014-1"-"124014-25"
SN  - 24700010
KW  - energy-momentum tensor;dimensionless parameter;numerical solution;isotropic perfect-fluid spheres
UR  - https://journals.aps.org/prd/abstract/10.1103/PhysRevD.106.124014
N2  - 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.
ER  - 

PAPPAS, Thomas, Nelson Camilo POSADA AGUIRRE a Zdeněk STUCHLÍK. Extended Tolman III and VII solutions in f (R, T) gravity: Models for neutron stars and supermassive stars. \textit{Physical Review D}. 2022, roč.~106, č.~12, s.~''124014-1''-''124014-25'', 25 s. ISSN~2470-0010. Dostupné z: https://dx.doi.org/10.1103/PhysRevD.106.124014.