  In this paper, we develop a new relativistic compact stellar model for a
spherically symmetric anisotropic matter distribution. The model has been
obtained through generating a new class of solutions by invoking the Tolman
{\em ansatz} for one of the metric potentials $g_{rr}$ and a physically
reasonable selective profile of radial pressure. We have matched our obtained
interior solution to the Schwarzschild exterior spacetime over the bounding
surface of the compact star. These matching conditions together with the
condition of vanishing the radial pressure across the boundary of the star have
been utilized to determine the model parameters. We have shown that the central
pressure of the star depends on the parameter $p_0$. We have estimated the
range of $p_0$ by using the recent data of compact stars 4U 1608-52 and Vela
X-1. The effect of $p_0$ on different physical parameters e.g., pressure
anisotropy, the subliminal velocity of sound, relativistic adiabatic index etc.
have also been discussed. The developed model of the compact star is
elaborately discussed both analytically and graphically to justify that it
satisfies all the criteria demanded a realistic star. From our analysis, we
have shown that the effect of anisotropy becomes small for higher values of
$p_0$. The mass-radius (M-R) relationship which indicates the maximum mass
admissible for observed pulsars for a given surface density has also been
investigated in our model. Moreover, the variation of radius and mass with
central density has been shown which allow us to estimate central density for a
given radius (or mass) of a compact star.
