Durgapal-Fuloria Bose-Einstein condensate stars within $ f(R,T) $ gravity theory

TL;DR

This paper models Bose-Einstein condensate stars within $f(R,T)$ gravity using the Durgapal-Fuloria metric, demonstrating stability and realistic features influenced by the coupling constant and metric parameters.

Contribution

It introduces new stable BEC star solutions in $f(R,T)$ gravity with detailed analysis of energy conditions and stability criteria, enhancing understanding of such stars in modified gravity.

Findings

Model satisfies energy conditions and stability criteria.

Coupling constant and metric parameters significantly affect stellar structure.

Results indicate realistic and stable BEC star configurations in $f(R,T)$ gravity.

Abstract

This manuscript studies the Bose-Einstein condensate (BEC) stars in the light of $ f(R,T) $ gravity here with Durgapal-Fuloria (DP) metric ansatz. The function under this study features as $ f(R,T) = R + 2\eta T $, where $ \eta $ represents the coupling constant. With the help of it, we have formulated a stellar model describing the isotropic matter here within. Our analysis covers energy conditions, equation of state (EoS) parameter and gradients of the energy-momentum tensor components for a valid BEC stellar framework within $ f(R,T) $ gravitational theory with satisfactory results. The model's stability has been validated via multiple stability criteria viz., the velocity of sound, study of adiabetic index and surface redshift where all are found to be lying within the acceptable range for our stellar model. Thus in all the cases we have found our model to be stable and realistic. From the graphical representations the impact of the coupling constant and the parameter of the DP metric potential are clearly visible. Thus we can state that with all the above-mentioned features we have introduced new stellar solutions for BEC stars with enhanced precise results in this modified gravity.