Modeling of Stellar solutions in Einstein–Gauss–Bonnet gravity

This article addresses an entirely novel class of stable compact stellar configurations under Einstein–Gauss–Bonnet gravity. To analyze the compact objects, we have taken into account spherically symmetric metric and adopted the Krori–Barua geometries. For this theoretical framework to accommodate neutron stars, the incorporation of the Gauss–Bonnet term is very important. Numerous physical characteristics of compact models, involving material variable, and its stability, have been thoroughly examined for Gauss–Bonnet coupled parameter. We also examine the stability of these stellar models while taking into consideration a variety of parameter values. Additionally, we delve into an exploration of the hydrostatic equilibrium of the compact system, achieved by utilizing a modified form of Tolman–Oppenheimer–Volkoff equation. Furthermore, we have assessed the stability of the solution by examining the square of the speed of sound velocity, the adiabatic index, and its critical values. In addition to this, we demonstrate a correlation inside mass and radius to derive the values of compactness factor and surface redshift of our obtained model. This comprehensive approach allows us to ascertain that the obtained stellar model attach to the fundamental physical requisites essential for a viable and physically meaningful stellar object.