https://doi.org/10.1140/epjc/s10052-023-11562-3
Regular Article - Theoretical Physics
Charged strange star model in Tolman–Kuchowicz spacetime in the background of 5D Einstein–Maxwell–Gauss–Bonnet gravity
1
Department of Mathematics, Sarat Centenary College, Dhaniakhali, 712 302, Hooghly, West Bengal, India
2
Astrophysics Research Centre, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Private Bag X54001, 4000, Durban, South Africa
3
Laboratory of High Energy Physics and Condensed Matter, Department of Physics, Faculty of Sciences Aïn Chock, Hassan II University of Casablanca, B.P. 5366 Maarif, 20100, Casablanca, Morocco
4
Department of Physics, Faculty of Sciences, Ibn Tofail University, P.O. Box 133, 14000, Kenitra, Morocco
5
Abdus Salam International Centre for Theoretical Physics, Miramare, 34151, Trieste, Italy
b
abdelghani.errehymy@gmail.com
Received:
29
March
2023
Accepted:
27
April
2023
Published online:
11
May
2023
In this article, we provide a new model of static charged anisotropic fluid sphere made of a charged perfect fluid in the context of 5D Einstein–Maxwell–Gauss–Bonnet (EMGB) gravity theory. To generate exact solutions of the EMGB field equations, we utilize the well-behaved Tolman–Kuchowicz (TK) ansatz together with a linear equation of state (EoS) of the form 
, (where 
and 
are constants). Here the exterior space-time is described by the EGB Schwarzschild metric. The Gauss–Bonnet Lagrangian term 
is coupled with the Einstein–Hilbert action through the coupling constant 
. When 
, we obtain the general relativity (GR) results. Here we present the solution for the compact star candidate EXO 1785-248 with mass
; radius 
km. respectively. We analyze the effect of this coupling constant on the principal characteristics of our model, such as energy density, pressure components, anisotropy factor, sound speed etc. We compare these results with corresponding GR results. Moreover, we studied the hydrostatic equilibrium of the stellar system by using a modified Tolman–Oppenheimer–Volkoff (TOV) equation and the dynamical stability through the critical value of the radial adiabatic index.The mass-radius relationship is also established to determine the compactness factor and surface redshift of our model. In this way, the stellar model obtained here is found to satisfy the elementary physical requirements necessary for a physically viable stellar object.
© 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/.
Funded by SCOAP3. SCOAP3 supports the goals of the International Year of Basic Sciences for Sustainable Development.
