The equilibrium configurations of rigidly rotating white dwarfs and neutron stars are calculated using the Harrison-Wheeler and the Tsuruta-Cameron V1 equations of state, along with the general-relativistic equations of structure. The equations of structure used are the exact relativistic equations with one ex- ception: they have been expanded in powers of the angular velocity ~2, and terms of higher order than ~ have been neglected. The equilibrium configurations of slowly rotating supermassive stars are also calculated
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Hartle et al. (1968) studied this question.