Relativistic stellar structures can be obtained both analytically and by computation, but all these models do not stand the tests of physical reality. It is shown that for a physically reasonable solution dρ/dr ∝-r and d(e v /dr ∝r near the centre, d(P/ρ)/dr -(P/ρ). If we change the variabler tox=Cr 2, whereC is a constant, the field equations are reduced to a form which is easier to solve. A new set of exact solutions is obtained by consideringe v ∝(1-x) n . Also, a method has been given to obtain generalized solution. It is shown that the solution discussed by Durgapal and Rawat (1980) is the only exact solution which in its most generalized form for a given density distribution stands all the tests of physical reality and for which both (P/ρ) and (dP/dρ) decrase with increasing value ofr. Neutron star model is proposed by assuming ρ>-2×1014g cm−3. Two specific cases are considered, viz.,P<-1/3ρ and dP/dρ<-1, respectively. The structures are found to be bound and stable under radial perturbations. The models have been studied for slow rotation and the mass of the Crab pulsar has been estimated for different mechanisms.