Minimally deformed anisotropic stars in dark matter halos under EGB-action

S. K. Maurya; Abdelghani Errehymy; Ksh. Newton Singh; Nuha Al-Harbi; Kottakkaran Sooppy Nisar; Abdel-Haleem Abdel-Aty

doi:10.1140/epjc/s10052-023-12127-0

2023 Impact factor 4.2

Particles and Fields

Open Access

Eur. Phys. J. C (2023) 83: 968
https://doi.org/10.1140/epjc/s10052-023-12127-0

Regular Article - Theoretical Physics

Minimally deformed anisotropic stars in dark matter halos under EGB-action

S. K. Maurya¹^a, Abdelghani Errehymy², Ksh. Newton Singh³, Nuha Al-Harbi⁴, Kottakkaran Sooppy Nisar⁵ and Abdel-Haleem Abdel-Aty⁶

¹ Department of Mathematical and Physical Sciences, College of Arts and Sciences, University of Nizwa, Nizwa, Sultanate of Oman
² Astrophysics Research Centre, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Private Bag X54001, 4000, Durban, South Africa
³ Department of Physics, National Defence Academy, Khadakwasla, 411023, Pune, India
⁴ Department of Physics, Faculty of Applied Sciences, Umm Al-Qura University, Makkah, Saudi Arabia
⁵ Department of Mathematics, College of Science and Humanities in Alkharj, Prince Sattam bin Abdulaziz University, Al Kharj, Saudi Arabia
⁶ Department of Physics, College of Sciences, University of Bisha, P.O. Box 344, 61922, Bisha, Saudi Arabia

^a sunil@unizwa.edu.om

Received: 25 August 2023
Accepted: 8 October 2023
Published online: 27 October 2023

Abstract

In this paper, we introduce an anisotropic model using a dark matter (DM) density profile in Einstein–Gauss–Bonnet (EGB) gravity using a gravitational decoupling method introduced by Ovalle (Phys Rev D 95:104019, 2017), which has provided an innovative approach for obtaining solutions to the EGB field equations for the spherically symmetric structure of stellar bodies. The Tolman and Finch–Skea (TFS) solutions of two metric potentials, $g_{tt}$ $g_{tt}$ and $g_{rr}$ $g_{rr}$ , have been used to construct the seed solution. Additionally, the presence of DM in DM halos distorts spacetime, causing perturbations in the $g_{rr}$ $g_{rr}$ metric potential, where the quantity of DM is determined by the decoupling parameter $β$ $\beta$ . The physical validity of the solution, along with stability and equilibrium analysis, has also been performed. Along with stability and equilibrium analysis, the solution’s physical validity has also been examined. Additionally, we have shown how both constants affect the physical characteristics of the solution. Using a $M - R$ $$M{-}R$$ diagram, it has been described how the DM component and the GB constant affect the maximum permissible masses and their corresponding radii for various compact objects. Our model predicts the masses beyond the $2 M_{⊙}$ $2~M_{\odot }$ and maximum radii $11 . 92_{- 0.01}^{+ 0.02}$ $11.92^{+0.02}_{-0.01}$ and $12 . 83_{- 0.02}^{+ 0.01}$ $12.83^{+0.01}_{-0.02}$ for larger value of $α$ $\alpha$ under density order $10^{15} g / {cm}^{3}$ $10^{15}~\text {g}/\text {cm}^3$ and $10^{14} g / {cm}^{3}$ $10^{14}~\text {g}/\text {cm}^3$ , respectively, while the radii become $11 . 96_{- 0.01}^{+ 0.01}$ $11.96^{+0.01}_{-0.01}$ and $12 . 81_{- 0.02}^{+ 0.01}$ $12.81^{+0.01}_{-0.02}$ for larger value of $β$ $\beta$ .

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