A Spherical Relativistic Anisotropic Compact Star Model

Abstract

We provide solutions to Einsteins field equations for a model of a spherically symmetric anisotropic fluid distribution, relevant to the description of compact stars. The central matter-energy density, radial and tangential pressures, red shift and speed of sound are positive definite and are decreasing monotonically with increasing radial distance from the center of matter distribution of astrophysical object. The causality condition is satisfied for complete fluid distribution. The central value of anisotropy is zero and is increasing monotonically with increasing radial distance from the center of the distribution. The adiabatic index is increasing with increasing radius of spherical fluid distribution. The stability conditions in relativistic compact star are also discussed in our investigation. The solution is representing the realistic objects

Linear and Riccati equations in generating functions for stellar models in general relativity

“…This works when the fluid is anisotropic in general. Such models were discussed in [72], [73], [74], [75], [76], [77], [78], [79], [80].…”

Charged stellar model with three layers

“…Importantly, the field equations are utilized to investigate different structures, behaviors and properties of stellar spheres relevant to astrophysical studies. They have drawn the attention and interest of researchers to develop relativistic 310-2 A. S. Lighuda et al: Charged Stellar Model with Three Layers stellar models in static or non-static spherically symmetric spacetime (Fulara & Sah 2018). A variety of mathematical approaches has been used to solve the system of field equations to investigate the physical features of superdense stellar objects (Tiwari 2010).…”