Anisotropic models for compact stars

TL;DR

This paper develops an anisotropic model for compact stars by extending a known perfect fluid solution, incorporating anisotropy through metric potentials, and validating the model against observed stellar properties.

Contribution

It introduces an anisotropic analogue of a classic perfect fluid solution using a novel contraction method of the anisotropic factor, and compares the results with real compact star data.

Findings

Model satisfies physical features of compact stars

Applicable to strange stars and white dwarfs

Validates anisotropic approach for stellar modeling

Abstract

In the present paper we obtain an anisotropic analogue of Durgapal-Fuloria (1985) perfect fluid solution. The methodology consists of contraction of anisotropic factor $\Delta$ by the help of both metric potentials $e^{\nu}$ and $e^{\lambda}$. Here we consider $e^{\lambda}$ same as Durgapal-Fuloria (1985) whereas $e^{\nu}$ is that given by Lake (2003). The field equations are solved by the change of dependent variable method. The solutions set mathematically thus obtained are compared with the physical properties of some of the compact stars, strange star as well as white dwarf. It is observed that all the expected physical features are available related to stellar fluid distribution which clearly indicate validity of the model.