Compact Relativistic Stars under Karmarkar Condition

TL;DR

This paper derives new solutions for relativistic star models under the Karmarkar condition, demonstrating their applicability to real pulsars and verifying physical plausibility through numerical and graphical analysis.

Contribution

It introduces a novel class of solutions for Einstein's field equations using a specific metric ansatz under the Karmarkar condition, applicable to observed pulsars.

Findings

Model can accommodate several observed pulsars.

Solutions satisfy all physical and energy conditions.

Physical parameters are consistent with realistic stellar objects.

Abstract

A class of new solutions for Einstein's field equations, by choosing the ansatz $e^{\lambda(r)}=\frac{1+ar^{2}}{1+br^{2}}$ for metric potential, are obtained under Karmarkar condition. It is found that a number of pulsars like 4U 1820-30, PSR J1903+327, 4U 1608-52, Vela X-1, PSR J1614-2230, Cen X-3 can be accomodated in this model. We have displayed the nature of physical parameters and energy conditions throughout the distribution using numerical and graphical methods for a particular pulsar 4U 1820-30 and found that the solution satisfies all physical requirements.