Models of quintessence compact stars in Rastall gravity consistent with observational data

Abstract

This work is devoted to present a new solution of field equations in the Rastall paradigm for isotropic matter content with quintessence field specified by the parameter $$\omega _q$$ with the condition $$-1<\omega _q<-\frac{1}{3}$$ . In order to obtain relativistic analytic solution, we used the Krori and Barua (KB) insatz in the static and spherically symmetric geometry. The obtained results analyzed analytically and graphically for the physical assessment. It is shown that for a suitable choice of coupling parameter, the original results in the standard general relativity (GR) can be retrieved. We provide a comparative study of acquired results in both the aspects, graphically and numerically with the observational evidences and GR counterpart. The comparative study shown that our obtained model is in good concurrence with the observational data in comparison with the GR. For this whole analysis, we considered five different compact stars namely, SAX J1808-3658 (SSI), Vela X-12, Her X-1, PSR J1416-2230 and 4U 1820-30 with radii 7.07 km, 9.99 km, 7.7 km, 10.3 km and 10 km, respectively. To check the viability of the presented model, we investigate different physical parameters such as energy conditions, stability analysis (via. sound speed and adiabatic index), Buchdahl limit, hydrostatic equilibrium of forces. We found that presented model is totally stable and well consistent with the plausible physical conditions.