A general numerical method is developed for constructing evolutionary sequences of threedimensional, axisymmetric, barytropic equilibrium configurations taking detailed account of angular-momentum transport by a nonconstant isotropic viscosity. Nonmagnetic, zero-temperature white-dwarf models in rapid differential rotatioh are considered as a particular application. Relevant properties of such stars are discussed, including contributions to the viscosity due to the ions and electrons. Subject headings: interiors, stellar - rotation, stellar - stellar evolution - white dwarf stars
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R. H. Durisen (1973) studied this question.