https://doi.org/10.1140/epjp/s13360-022-03458-0
Regular Article
Anisotropic electrically charged stars in f(Q) symmetric teleparallel gravity
1
Astrophysics Research Centre, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Private Bag X54001, 4000, Durban, South Africa
2
Laboratory of High Energy Physics and Condensed Matter, Department of Physics, Faculty of Sciences Aïn Chock, Hassan II University of Casablanca, P.O. Box 5366, Maarif, 20100, Casablanca, Morocco
3
Department of Mathematics, Shanghai University, 200444, Shanghai, Shanghai, People’s Republic of China
4
Department of Physics, Zhejiang Normal University, 321004, Jinhua, People’s Republic of China
5
Department of Mathematical and Physical Sciences, College of Arts and Sciences, University of Nizwa, Nizwa, Sultanate of Oman
6
Department of Physics, College of Sciences, University of Bisha, P.O. Box 344, 61922, Bisha, Saudi Arabia
7
Department of Physics, Faculty of Science, Al-Azhar University, 71524, Assiut, Egypt
Received:
3
August
2022
Accepted:
2
November
2022
Published online:
5
December
2022
In this paper, we investigate the properties of anisotropic, spherically symmetric compact stars, especially, electrically charged strange stars in f(Q) symmetric teleparallel gravity. Those stars are hypothesized to be composed of strange quark matter, whose distribution is controlled by the MIT-Bag model equation of state (EoS), which correlates density and pressure by incorporating the Bag constant (which balances the inward-directed Bag pressure). In contrast, the form of electrical charge distribution is chosen to be 
, where k is the charge intensity for exhibiting the charged nature of matter distributions. When considering this theory, the unidentified constraints are evaluated by the matching of interior spacetime with the Reissner–Nordström exterior geometry corresponding to Tolman models. In particular, with the assumption that radial pressure at the stellar surface is vanishing, the radii of compact star candidates viz., GW190814, 
, and 
are predicted using their observed masses. The physical viability and hydrostatic equilibrium along with the dynamical stability of the resulting solution through graphical behavior of matter variables, energy constraints, modified TOV equation, adiabatic index, and causality condition were also tested in order to describe the realistic models. Conclusively, our findings indirectly support the existence of electrically charged super-massive pulsars in f(Q) gravitational theory.
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