https://doi.org/10.1140/epjc/s10052-024-13735-0
Regular Article - Theoretical Physics
Constructing stellar solutions with spherical symmetry through quadratic anisotropy in f(Q) gravity
1
Department of Mathematics and Statistics, Deen Dayal Upadhyaya Gorakhpur University, Gorakhpur, India
2
Department of Mathematical and Physical Sciences, College of Arts and Sciences, University of Nizwa, 616, Nizwa, Oman
3
Astrophysics Research Centre, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Private Bag X54001, 4000, Durban, South Africa
4
Pacif Institute of Cosmology and Selfology (PICS), Sagara, 768224, Sambalpur, Odisha, India
5
Department of General and Theoretical Physics, L.N. Gumilyov Eurasian National University, 010008, Astana, Kazakhstan
a
abdelghani.errehymy@gmail.com
b
krmyrzakulov@gmail.com
Received:
23
September
2024
Accepted:
26
December
2024
Published online:
25
January
2025
This article examines anisotropic models to characterize compact stars (CSs) in the context of modified f(Q) gravity theory. To achieve this, we employ the linear functional form . A physically meaningful metric potential
is considered, and a quadratic form of anisotropy is utilized to solve the Einstein field equations in closed form. This class of solutions is then applied to characterize observed pulsars from various perspectives. In the scope of f(Q) gravity, we address the Darmois–Israel junction requirements to guarantee a smooth matching of the inner metric with the external metric (Schwarzschild (Anti-) de Sitter solution) at the boundary hypersurface. By applying these junction conditions, we determine the model parameters involved in the solutions. Additionally, this study evaluates the physical viability and dynamical stability of the solution for different values of the f(Q)-parameter
within the compact star (CS). The mass–radius relationships associated with observational constraints are analyzed for several compact stars, including Vela X-1, PSR J1614-2230, and PSR J0952-0607. The investigation indicates that the estimated radius of the compact object PSR J0952-0607, with mass
, is around
km for a particular parameter value of
, and the moment of inertia for the de Sitter space is determined as
. The
curve shows greater sensitivity to the stiffness of the equation of state than the
curve, reinforcing our conclusion about the
framework’s responsiveness. Finally, we predicted the corresponding radii and moments of inertia for various values of
based on the
and
curves.
© The Author(s) 2025
Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/.
Funded by SCOAP3.