  This paper offers novel quintessence compact relativistic spherically
symmetrical anisotropic solutions under the recently developed Ricci inverse
gravity Amendola et al., 2020), by employing Krori and Barua gravitational
potentials, $Ar^2=\nu(r), ~\&~Br^2+C=\mu(r)$ (with A, B, and C being real
constants). For this objective, a specific explicit equation of state,
connecting energy density and radial pressure, i.e., $p_r=\omega\rho$, such
that $0<\omega<1$, has been utilized with an anisotripic fluid source. Ricci
inverse field equations are used to find the exclusive expressions of the
energy density, radial and tangential stresses, and the quintessence energy
density, the critical physical attributes reflecting the exceptional conduct of
extremely dense matter configuration. For the observatory source stars $Her
X-1$, $SAX J 1808.4-3658$ and $4U 1820-30$, all the important physical
quantities like energy densities, tangential and radial pressures, energy
conditions, gradients, anisotropy, redshift and mass-radius functions, and
stellar compactness have been worked out and analyzed graphically. It has been
concluded that all of the stellar formations under consideration remain free
from any undesirable central singularity and are stable.
