We present two new families of global equilibrium solutions of the Vlasov‐Poisson equations, intended to model collisionless but quasi‐relaxed stellar systems, such as globular clusters, characterized by the presence of internal rotation. The first one is an extension to the case of ax‐isymmetric equilibria flattened by solid‐body internal rotation of the well‐known family of King models, defined by a quasi‐Maxwellian distribution function. In turn, the second family is characterized by differential rotation, designed to be rigid in the center and to vanish in the outer parts of the stellar system, where the energy truncation is effective. The physical scenario that inspired the definition of the families is discussed in the more general context of the dynamical evolution of quasi‐relaxed stellar systems and a preliminary analysis of their intrinsic properties is provided.

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