An isotropic compact stellar model in curvature coordinate system consistent with observational data

TL;DR

This paper develops an isotropic relativistic stellar model using Vaidya-Tikekar metric parameters, accurately matching observational data and analyzing physical stability criteria for various compact stars.

Contribution

It introduces a new perfect fluid model with specific metric parameters that fit observational data and satisfy all physical and stability conditions for compact stars.

Findings

Model fits observational data of multiple compact stars

Obeys all physical and stability criteria

Provides a framework for analyzing other isotropic compact objects

Abstract

This paper investigates a spherically symmetric compact relativistic body with isotropic pressure profiles within the framework of general relativity. In order to solve the Einstein's field equations, we have considered the Vaidya-Tikekar type metric potential, which depends upon parameter K. We have presented a perfect fluid model, considering K<0 or K>1, which represent compact stars like SMC X-1, Her X-1, 4U 1538-52, SAX J1808.4-3658, LMC X-4, EXO 1785-248 and 4U1820-30, to an excellent degree of accuracy. We have investigated the physical features such as the energy conditions, velocity of sound, surface redshift, adiabatic index of the model in detail and shown that our model obeys all the physical requirements for a realistic stellar model. Using the Tolman-Oppenheimer-Volkoff equations, we have explored the hydrostatic equilibrium and the stability of the compact objects. This model also fulfils the Harrison-Zeldovich-Novikov stability criterion. The results obtained in this paper can be used in analyzing other isotropic compact objects.