Eur. Phys. J. Plus (2025) 140: 348
https://doi.org/10.1140/epjp/s13360-025-06280-6

Regular Article

A new generic class of charged stellar structure in general relativity verified by observational data

¹ Department of Mathematics, College of Science, King Saud University, P.O. Box 22452, 11495, Riyadh, Kingdom of Saudi Arabia
² Department of Mathematics, Bahauddin Zakariya University, Vehari Campus, 61100, Vehari, Pakistan
³ Research Center of Astrophysics and Cosmology, Khazar University, 41 Mehseti Street, AZ1096, Baku, Azerbaijan
⁴ Department of Physics, College of Science, Jazan University, P.O. Box 114, Jazan, Kingdom of Saudi Arabia

^a dr.rizwanshahzad@bzu.edu.pk
^b makermi@jazanu.edu.sa

Received: 19 March 2025
Accepted: 28 March 2025
Published online: 29 April 2025

Abstract

In this work, we propose a new generic class of charged stellar structures in general relativity (GR), which is consistent with observational data. The geometry considered in this study is the static and spherically symmetric with an anisotropic matter configuration inside the geometry. To make the system of governing field equations solvable, we considered the phenomenological MIT bag model equation of state. In this model, the relationship between the density profile ($\rho$) and the radial pressure ($P_r$) is represented by the equation $P_r(r)=\frac{1}{3}(\rho -4B_g)$. The governing Einstein–Maxwell field equations are solved by taking the Tolman–Durgapal-V (TD-V) metric potentials into account, in which the Tolman metric potential (Tolman, Phys Rev 55:364, 1939) is defined by $e^{\lambda (r)}=(1+a{r}^2+b{r}^4)$ and the Durgapal-V metric potential (Durgapal, Phys Rev 15:2637, 1982) is defined by $e^{\nu (r)}=B{(1+C{r}^2)}^5$. The parameters a, b, B, and C included in these potentials are calculated by comparing the Reissner–Nordstr$\ddot{o}m$ line element as an external geometry at the stellar surface corresponding to the interior space–time. In our study, we perform an extensive validation of the proposed model to verify its legitimacy as a physically consistent compact object under the framework of GR by considering a dozen compact star candidates as representatives of a large class of compact stellar structure. The results demonstrate that the model maintains stable behavior without singularities and successfully represents a diverse range of observed compact objects in astrophysical contexts. This thorough assessment ensures that the model complies with critical physical standards, bolstering its applicability in understanding compact star dynamics.