A generalised embedding class one static solution describing anisotropic fluid sphere.

In the present article, the Eiesland condition has been used to obtain a new solution for compact star model by considering a non-singular well behaved gravitational potential of the form e λ (r) = 1 + a r 2 [ 1 + tanh (b r 2 + c) ] n in the framework of anisotropic matter distribution. The solution so obtained is physically acceptable, which is exploited to compare the predicted masses and radii of known compact object as EXO 1785-248 (M = 1.3 M ⊙ ) for n = 3 to 15. Moreover, the obtained solution satisfies the causality condition, Herrera cracking criterion, Tolman-Oppenheimer-Volkoff (TOV) equation, and adiabatic index Γ including all energy conditions. It is noted that the velocity of sound is increasing at n = 3 and start decreasing when n ≥ 6 which shows that the parameter n plays an important role to describe a well-behaved solution for anisotropic compact object. The moment of inertia (I) is also obtained by Bejger-Haensel formula for n = 3 to 15. In addition to that, the maximum mass for the compact star has been discovered via. M − R curve for different values of n . [ABSTRACT FROM AUTHOR]