  In the present paper we obtain an anisotropic analogue of Durgapal-Fuloria
(1985) perfect fluid solution. The methodology consists of contraction of
anisotropic factor $\Delta$ by the help of both metric potentials $e^{\nu}$ and
$e^{\lambda}$. Here we consider $e^{\lambda}$ same as Durgapal-Fuloria (1985)
whereas $e^{\nu}$ is that given by Lake (2003). The field equations are solved
by the change of dependent variable method. The solutions set mathematically
thus obtained are compared with the physical properties of some of the compact
stars, strange star as well as white dwarf. It is observed that all the
expected physical features are available related to stellar fluid distribution
which clearly indicate validity of the model.
