Embedding class 1 model of anisotropic fluid spheres in f(R,T) gravity

In this paper, we present new physically viable interior solutions of the Einstein field equations for static and spherically symmetric anisotropic compact stars satisfying the Karmarkar condition. For presenting the exact solutions, we provide a new suitable form of one of the metric potential functions. Obtained solutions satisfy all the physically acceptable properties of realistic fluid spheres and hence solutions are well-behaved and representing matter distributions are in equilibrium state and potentially stable by satisfying the TOV equation and the condition on stability factor, adiabatic indices. We analyze the solutions for two well-known compact stars Vela X-1 (Mass = 1.77 M[Formula: see text], R = 9.56 km) and Cen X-3 (Mass = 1.49 M[Formula: see text], R = 9.17 km).

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Some new Wyman–Leibovitz–Adler type static relativistic charged anisotropic fluid spheres compatible to self-bound stellar modeling

The European Physical Journal C ◽

10.1140/epjc/s10052-015-3737-6 ◽

2015 ◽

Vol 75 (11) ◽

Cited By ~ 25

Author(s):

Mohammad Hassan Murad ◽

Saba Fatema

Keyword(s):

Anisotropic Fluid ◽

Fluid Spheres

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Modeling of immense gravity objects via generalized solution of Einstein’s field equations

International Journal of Modern Physics D ◽

10.1142/s0218271819501347 ◽

2019 ◽

Vol 28 (10) ◽

pp. 1950134

Author(s):

Kiran Pant ◽

Pratibha Fuloria

Keyword(s):

Mass Formula ◽

Compact Star ◽

Generalized Solution ◽

Energy Conditions ◽

Anisotropic Fluid ◽

Field Equations ◽

Star Models ◽

Spacetime Manifold ◽

Class 1 ◽

Physical Features

In this paper, we generate a new generalized solution for modeling of compact anisotropic astrophysical configurations by using Karmarkar condition of embedded class 1 spacetime manifold. We demonstrate that the new solution satisfies all required physical conditions. We investigate several physical properties of compact star models, i.e. Vela X-1 (Mass [Formula: see text][Formula: see text], radius = [Formula: see text][Formula: see text]km), PSRJ [Formula: see text] (Mass [Formula: see text][Formula: see text], radius = [Formula: see text][Formula: see text]km) and PSRJ [Formula: see text] (Mass [Formula: see text][Formula: see text], radius = [Formula: see text][Formula: see text]km) in conformity with the observational data. The proposed solution is free from singularities, satisfies causality condition and displays well-behaved nature inside the anisotropic configurations. All energy conditions and hydrostatic equilibrium condition are well defined inside the anisotropic fluid spheres. The adiabatic index throughout the stellar interior is greater than [Formula: see text] and the compactification factor lies within the Buchdahl limit [Formula: see text]. We study the physical features of the solution in detail, analytically as well as graphically for compact star Vela X-1 with [Formula: see text] ranging from [Formula: see text] to [Formula: see text].

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