  We investigate a compact spherically symmetric relativistic body with
anisotropic particle pressure profiles. The distribution possesses
characteristics relevant to modeling compact stars within the framework of
general relativity. For this purpose, we consider a spatial metric potential of
Korkina and Orlyanskii [Ukr. Phys. J. 36, 885 (1991)] type in order to solve
the Einstein field equations. An additional prescription we make is that the
pressure anisotropy parameter takes the functional form proposed by Lake [Phys.
Rev. D 67, 104015 (2003)]. Specifying these two geometric quantities allows for
further analysis to be carried out in determining unknown constants and
obtaining a limit of the mass-radius diagram, which adequately describes
compact strange star candidates like Her X-1 and SMC X-1. Using the anisotropic
Tolman-Oppenheimer-Volkoff equations, we explore the hydrostatic equilibrium
and the stability of such compact objects. Then, we investigate other physical
features of this models, such as the energy conditions, speeds of sound and
compactness of the star in detail and show that our results satisfy all the
required elementary conditions for a physically acceptable stellar model. The
results obtained are useful in analyzing the stability of other anisotropic
compact objects like white dwarfs, neutron stars, and gravastars.
