Anisotropic compact stars: Constraining model parameters to account for physical features of tidal Love numbers

TL;DR

This paper introduces a new anisotropic star model with a linear equation of state, matching observational data and calculating tidal Love numbers to better understand the internal structure of compact stars.

Contribution

The study develops a novel anisotropic star model with specific metric ansatz and constrains parameters using observational data, enhancing understanding of tidal effects on compact stars.

Findings

Model parameters constrained by pulsar data

Calculated Love numbers consistent with observations

Physical viability confirmed for the proposed model

Abstract

In this paper, we develop a new class of models for a compact star with anisotropic stresses inside the matter distribution. By assuming a linear equation of state for the anisotropic matter composition of the star we solve the Einstein field equations. In our approach, for the interior solutions we use a particular form of the ansatz for the metric function $g_{rr}$. The exterior solution is assumed as Schwarzschild metric and is joined with the interior metric obtained across the boundary of the star. These matching of the metrices along with the condition of the vanishing radial pressure at the boundary lead us to determine the model parameters. The physical acceptability of the solutions has verified by making use of the current estimated data available from the pulsar 4U1608-52. Thereafter, assuming anisotropy due to tidal effects we calculate the Love numbers from our model and compare the results with the observed compact stars, viz. KS 1731- 260,4U 1608- 52,4U 1724- 207,4U 1820- 30,SAX J1748.9-2021 and EXO 1745-268. The overall situation confirms physical viability of the proposed approach,which can shed new light on the interior of the compact relativistic objects.