Pulsar PSR B0943+10 as an isotropic Vaidya-Tikekar type compact star : A comprehensive study

TL;DR

This study develops a detailed isotropic charged compact star model using the Vaidya-Tikekar metric, validating it with pulsar PSR B0943+10 data and confirming its physical stability and acceptability.

Contribution

It introduces a new isotropic charged star model based on the Vaidya-Tikekar metric, validated with observational data and stability criteria.

Findings

Model satisfies all physical conditions for compact stars.

The star model remains stable under various stability tests.

Data of pulsar PSR B0943+10 supports the model's validity.

Abstract

In this paper, we have constructed a model for well behaved isotropic compact star in the presence of charged perfect fluid, by considering a static and spherically symmetric metric in Schwarzschild's canonical coordinate system. To put the resulting differential equations into a closed system, we have employed the Vaidya & Tikekar (J. Astrophys. Astron. 3:325, 1982) form of the metric potential grr. The resulting energy-momentum components, i.e., energy density and pressure contain six constants; two of these are determined through the junction condition (matching the interior with the exterior Schwarzschild solution) and by the property of vanishing pressure on the boundary. The remaining constants are constrained by requirements of a real compact star. The physical acceptability of our model is tested using the data of the pulsar PSR B0943+10. Using graphical analysis and tabular information we have shown that our model obeys all the physical requirements. The stability of this model is evaluated using the Tolman-Oppenheimer-Volkoff equation, the adiabatic index and the Harrison-Zeldovich-Novikov Criterion and it has passed the evaluation.