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The Einstein-Maxwell (or Einstein) system of field equations plays asubstantial role in the modeling of compact stars. Although due to itsnon-linearity getting an exact solution for the system of field equations is adifficult task, the solutions of field equations have a long and rich history.It took a year for Karl Schwarzschild to obtain the first exact solution ofEinstein's field equations since general theory of relativity was published.The number of viable solutions has been growing since then. Many authors haveadopted several methods to obtain the solution. Different models have beenconstructed for a variety of applications. To produce feasible models ofcompact stars, a considerable amount of effort has been applied in gaining anunderstanding of the properties of anisotropic matter. Theoretical studyindicates that pressure within compact stars with extreme internal density andstrong gravity is mostly anisotropic. Anisotropy was found sufficient for thestudy of compact stars with the dense nuclear matter. It is claimed that it isimportant to consider the pressure experienced to be anisotropic wheneverrelativistic fluids are involved. In this review article, we have discusseddifferent ways of generating a static spherically symmetric anisotropic fluidmodel. The purpose of the article is to present a simple classification schemefor static and spherically symmetric anisotropic fluid solutions. The knownsolutions are reviewed and compartmentalized as per the proposed scheme so thatwe can illustrate general ideas about these solutions without being exhaustive.

The classification of interior solutions of anisotropic fluid configurations