  We present a model for compact stars in the low mass X-ray binaries(LMXBs)
and X-ray pulsars using a metric given by John J. Matese and Patrick G. Whitman
\citep{Matese and Whitman1980}. Here the field equations are reduced to a
system of two algebraic equations considering the isotropic pressure. Compact
star candidates 4U 1820-30(radius=10km) in LMXBs, and Her X-1(radius=7.7km),
SAX J 1808.4-3658(SS1)(radius=7.07km) and SAX J 1808.4-3658(SS2)(radius=6.35km)
in X-ray pulsars satisfy all the energy conditions, TOV-equation and stability
condition. From our model, we have derived mass($M$), central
density($\rho_{0}$), suface density($\rho_{b}$), central pressure($p_{0}$),
surface pressure($p_{b}$) and surface red-shift($Z_{s}$) of the above mentioned
stars, which are very much consistant with the observed/reported datas\citep{N.
K. Glendenning1997,Gondek2000}. We have also observe the adiabatic
index($\gamma$>4/3) of the above steller objects.
