  A family of solutions defining the interior of a static, spherically
symmetric, compact anisotropic star is described by considering a new form of
the equation of state (EOS). The analytic solution is derived by using the
Finch and Skea ansatz for the metric potential g_rr, which has a clear
geometric interpretation for the related background spacetime. The model
parameters are fixed by smooth matching of the interior solution to the
Schwarzschild exterior metric over the bounding surface of the compact star,
together with the requirement that the radial pressure vanishes at the
boundary. Data available for the pulsar 4U1802030 has been utilized to analyze
the physical viability of the developed model. The model is shown to be stable.
