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

Compact stellar model in Tolman space-time in presence of pressure anisotropy