Abstract
In this article, we have presented a static anisotropic solution of stellar compact objects for self-gravitating system by using minimal geometric deformation techniques in the framework of embedding class one space-time. For solving of this coupling system, we deform this system into two separate system through the geometric deformation of radial components for the source function lambda (r) by mapping: e^{-lambda (r)}rightarrow e^{-tilde{lambda }(r)}+beta ,g(r), where g(r) is deformation function. The first system corresponds to Einstein’s system which is solved by taking a particular generalized form for source function tilde{lambda }(r) while another system is solved by choosing well-behaved deformation function g(r). To test the physical viability of this solution, we find complete thermodynamical observable as pressure, density, velocity, and equilibrium condition via. TOV equation etc. In addition to the above, we have also obtained the moment of inertia (I), Kepler frequency (v), compression modulus (K_e) and stability for this coupling system. The M–R curve has been presented for obtaining the maximum mass and corresponding radius of the compact objects.
Highlights
4-dimensional Riemannian manifold, which is called spacetime, (ii) the curvature related with the metric is related to the matter by Einstein’s field equations (EFE)
The GD was developed by Ovalle [25,26] as a consequence of the Minimal Geometric Deformation (MGD)
It is noted that the presence of this extra source Θμν in Eq (8) produce an anisotropies in self gravitating system that can be a scalar, vector or tensor field
Summary
4-dimensional Riemannian manifold, which is called spacetime, (ii) the curvature related with the metric is related to the matter by Einstein’s field equations (EFE). The method of gravitational decoupling by Minimal Geometric Deformation (MGD) is a great and powerful technique that extends known solutions into more difficult situations. [8], Gabbanelli et al have extended isotropic Durgapal–Fuloria solution in the anisotropic domain while Ovalle and his collaborators [9] have shown that how a spherically symmetric fluid modifies the Schwarzschild vacuum solution and necessity of anisotropy in the fluid In this connection, several other authors have used the MGD approach to discover the more complex solution which can be seen in the following Refs. The purpose of this article is to the study of minimally deformed solution for class one space-time by using gravitational decoupling method that gives a generalised solution for anisotropic compact star models.
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