  In the present work, we study a new model of anisotropic compact stars in the
regime of Rastall theory. To solve the Rastall field equations we have used the
Karori and Barua (KB) ansatz along with the quintessence dark energy
characterized by a parameter $\omega_{q}$ with $-1<\omega_{q}<-\frac{1}{3}$. We
present a comparative study to demonstrate the physical acceptance of our
proposed model. We compare the numerical values of physical parameters obtained
from our model with those of general relativity ($GR$) model given by Bhar
\cite{1} and observe that our model is more compatible (for some chosen values
of Rastall dimensionless parameter $\gamma=\kappa\lambda$) with observational
data than $GR$ model. For this analysis we have consider four different compact
stars, $SAX J1808-3658 (SSI)$, $4U 1820-30$, $Vela X-12$ and $PSR J1416-2230$
with radii $7.07km$, $10km$, $9.99km$ and $10.3km$, respectively. In this
investigation we also present some physical aspects of the proposed model
necessary to check the validity of the model and inferred that our model is
acceptable physically and geometrically.
