Research PaperNo Access

A comparative analysis of self-consistent charged anisotropic spheres

Mushtaq Ahmad

National University of Computer and Emerging Sciences, Islamabad, Chiniot-Faisalabad Campus, Pakistan

E-mail Address: mushtaq.sial@nu.edu.pk

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G. Mustafa

Department of Physics, Zhejiang Normal University, Jinhua 321004, P. R. China

E-mail Address: gmustafa3828@gmail.com

Corresponding author.

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, and

M. Farasat Shamir

National University of Computer and Emerging Sciences, Islamabad, Lahore Campus, Pakistan

E-mail Address: farasat.shamir@nu.edu.pk

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https://doi.org/10.1142/S0217751X21502031Cited by:12 (Source: Crossref)

Abstract

This study is devoted to exploring the charged stellar structures under embedded space–time using the Karmarkar condition. For this, spherically symmetric space–time with the anisotropic source of fluid possessing an electric charge has been incorporated. Further, the Bardeen and Reissner–Nordstrom geometries have been employed as exterior space–time to calculate the values of the involved constants. The interior solutions of a stellar object have been worked out with the observational mass $M = 2.01 M_{⊙}$ $M = 2.01 M_{⊙}$ , and $R_{𝜖} = 9.1$ $R_{𝜖} = 9.1$ km. It is argued that the acquired solutions accomplish all the necessary conditions for self-consistent charged stars. It has been noted through the detailed graphical analysis that our obtained solutions are physically stable and self-consistent with the best degree of accuracy for $n \in [12, 15]$ $n \in [12, 15]$ , where parameter $n$ $n$ is involved in the model under discussion. Beyond this bound $12 \leq n \leq 15$ $12 \leq n \leq 15$ , the realistic solutions of stellar models under discussion could not be found. After perceiving the marginal dissimilarities between our proposed models in both cases, Andreasson’s limit $\sqrt{R_{𝜖}} / 3 + \sqrt{R_{𝜖} / 9 + q^{2} / 3 R_{𝜖}} \geq \sqrt{M}$ $\sqrt{R_{𝜖}} / 3 + \sqrt{R_{𝜖} / 9 + q^{2} / 3 R_{𝜖}} \geq \sqrt{M}$ , critically important for the stellar structures, has been achieved in both the models under investigation. Lastly, it is established that the parameter $n$ $n$ has a substantial effect on worked-out solutions under the employment of Bardeen and Reissner–Nordstrom’s stellar structures.

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