Relativistic solutions of anisotropic compact objects

Abstract

We present a class of new relativistic solutions with anisotropic fluid for compact stars in hydrostatic equilibrium. The interior space-time geometry considered here for compact objects are described by parameters namely, λ, k, A, R and n. The values of the geometrical parameters are determined here for obtaining a class of physically viable stellar models. The energy-density, radial pressure and tangential pressure are finite and positive inside the anisotropic stars. Considering some stars of known mass we present stellar models which describe compact astrophysical objects with nuclear density.

A conformally flat realistic anisotropic model for a compact star

“…The redshift Z throughout the star is obtained then from Eq. (9). The derivative of ν with respect to x, which enters the field equations, is…”

“…One of the first was given in [6], where some of the Tolman isotropic solutions [7] were modified to become anisotropic. Other followed recently [8], [9], [10], [11], [12], [13], [14].…”

Charged compact objects in f(R,T) gravity

“…Kalam et al 5 analyzed the relativistic modeling of anisotropic compact objects and checked the validity of energy conditions, anisotropy measurement and stability with quintessence dark energy (DE). For anisotropic distribution, Paul and Deb 6 formulated new relativistic solutions of compact stars which preserve the hydrostatic equilibrium.…”

Contraction of cold neutron star due to in the presence a quark core

“…It will be worthwhile to study the effects of the magnetic field [83][84][85][86], generalization of static compact objects to anisotropic [87][88][89][90][91][92], rotating [93][94][95][96][97][98][99][100][101][102], rapidly rotating [103][104][105][106][107][108][109][110] on the structure properties of neutron stars with a quark matter in core can be interesting topics. We leave these issues for future works.…”