Physical properties of a quintessence anisotropic stellar model in f(Q) gravity and the mass–radius relation

Piyali Bhar

doi:10.1140/epjc/s10052-023-11865-5

2023 Impact factor 4.2

Particles and Fields

Open Access

Eur. Phys. J. C (2023) 83: 737
https://doi.org/10.1140/epjc/s10052-023-11865-5

Regular Article - Theoretical Physics II

Physical properties of a quintessence anisotropic stellar model in f(Q) gravity and the mass–radius relation

Piyali Bhar^a

Department of Mathematics, Government General Degree College Singur, 712409, Hooghly, West Bengal, India

^a piyalibhar90@gmail.com

Received: 4 May 2023
Accepted: 23 July 2023
Published online: 19 August 2023

Abstract

In this article, we present a new family of solutions to the Einstein field equations of an uncharged spherically symmetric anisotropic matter distribution in the context of f(Q) gravity by choosing $f (Q) = Q + a Q^{2}$ $$f(Q)=Q+aQ^2$$ , a being the coupling constant. Along with the fundamental quintessence dark energy defined by the equation of state parameter $- 1 < ω_{q} < - \frac{1}{3}$ $-1<\omega _q<-\frac{1}{3}$ , we have generated the field equations in modified gravity. Using the linear relationship between radial pressure and energy density along with the Krori–Barua (KB) metric potential, we are able to solve the field equations. Next, we discuss the smooth matching between the exterior Schwarzschild spacetime and the interior spherically symmetric spacetime. We have presented a thorough physical analysis of several factors analytically and graphically to show the physical viability of our suggested model. For the compact star SAXJ 1808.4-3658, our entire graphical analysis was carried out in the context of our solutions for various values of the coupling constant connection to the f(Q) gravity. The influence of coupling constant “a” on different model parameters has been numerically determined and is presented in tabular form. We checked the radial and tangential sound speeds, the stability factor, the adiabatic index, etc. to determine whether our model was stable. It is evident from our analysis that the model is potentially stable when coupling constant $a \in [0, 5]$ $a \in [0,\,5]$ . The maximum allowable mass and radius from our present model have been obtained through the mass–radius ( $M - R$ $$M-R$$ ) plot for different values of a.

© The Author(s) 2023

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/.