Numerous scholars have been inspired to investigate the geometry of stellar interior sections by the phenomenon of supernovae stars producing unusual stars through gravitational collapse [1,2]. The Einstein field equations are helpful in general relativity when studying the gravitational behavior and physical properties of compact stellar entities, such as black holes, neutron stars, and white dwarfs, which are examples of star remnants [3-5]. Numerous models have been developed using the Einstein-Maxwell field equations and used to study various aspects of compact star objects [6–18]. The main idea of these models is that the field equations are practical and may be used as instruments to produce astrophysically meaningful conclusions.

Schwarzschild [3] produced the first solution to Einstein's field equations, known as the Schwarzschild solution, which was one of the revolutionary advances in the theory of general relativity. By assuming that the electric field, the mass's rotational momentum, and the cosmological constant are all zero, this solution explains the gravitational field outside of a spherical mass. Understanding how huge objects behave and interact with gravity has been made possible thanks in large part to this method. 

In order to investigate a variety of properties, including as their mass, charge, structure, and stability, modeling compact stellar objects has grown in popularity and importance [19]. With a variety of state equations, such as the linear equation of state [20-26], quadratic equation of state [27-30], polytropic equation of state [31-32], and Van der Waals equation of state [33-34], some plausible physical stellar models can be put forth.

For many astrophysics researchers, the investigation of anisotropy pressure in star objects in the presence of strong gravitational fields is a fundamentally important topic. Phase transitions are factors of neutron star evolution, according to Sokolov [18]. Anisotropy can also result from the presence of an electrical field [19]. Anisotropy can alter the structure of compact objects, according to Bowers and Liang [6]. Because radial forces of different signs arise in the star interior, disrupting the system balance, Herrera [11] concludes that pressure anisotropy affects matter stability. Anisotropy affects the structure and some physical characteristics of compact stars, including mass and compactness, according to Thirukkanesh and Ragel [35]. Furthermore, some studies have developed anisotropic models. (Mak and Harko [36], Malaver and Iyer [37], Thirukkanesh and Ragel [32], Takisa and Maharaj [31], Malaver [33–34], and Thirukkanesh and Ragel [35]).

The impact of electromagnetic fields on compact stellar bodies in a Buchdahl space time has been examined by Malaver et al [38]. With the metric potential put forth by Buchdahl, Malaver, et al [39] have identified a few physical characteristics for compact star objects in the framework of Einstein-Gauss-Bonnet gravity. The significance of Rank-n tensor time in quantifying gravity in quantum states with gravity and tensor time metrics has been the subject of numerous studies and talks by Iyer [40–41] in recent years. In these investigations, a novel method for combining General Relativity (GR) with Quantum Relativity (QR) is shown by the gradation of time tensors from rank-6 to rank-1 vectors in space time.

Using a linear equation of state with a particular metric function and taking pressure anisotropy into account, we developed new mathematical models for a compact star in this study. This is how the article is structured: we introduce Einstein's field equations for anisotropic fluid distribution in section 2. In section 3, we build novel models for charged anisotropic matter by selecting an electric field strength and gravitational potential that enable the solution of the field equations. The requirements for physical acceptability are covered in Section 4. Section 5 looks at these novel solutions' physical characteristics and validity. Section 6 presents the findings drawn from the outcomes of the computational implementations.

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