  A class of solutions of Einstein field equations satisfying Karmarkar
embedding condition is presented which could describe static, spherical fluid
configurations, and could serve as models for compact stars. The fluid under
consideration has unequal principal stresses i.e. fluid is locally anisotropic.
A certain physically motivated geometry of metric potential has been chosen and
codependency of the metric potentials outlines the formation of the model. The
exterior spacetime is assumed as described by the exterior Schwarzschild
solution. The smooth matching of the interior to the exterior Schwarzschild
spacetime metric across the boundary and the condition that radial pressure is
zero across the boundary lead us to determine the model parameters. Physical
requirements and stability analysis of the model demanded for a physically
realistic star are satisfied. The developed model has been investigated
graphically by exploring data from some of the known compact objects. The
mass-radius (M-R) relationship that shows the maximum mass admissible for
observed pulsars for a given surface density has also been investigated.
Moreover, the physical profile of the moment of inertia (I) thus obtained from
the solutions is confirmed by the Bejger-Haensel concept.
