ABSTRACT
The structure equations of rotating compact stars are considerably more complicated that those of non-rotating compact stars. This chapter describes the derivation of the stellar structure equations of compact, rotationally deformed stars. It presents the most of the mathematical expressions that follow from Albert Einstein’s equations for a rotating stellar configuration. In contrast to Newtonian theory, however, the inertial frames inside a general relativistic fluid are not at rest with respect to the distant stars. In cold neutron stars, superfluid eddy viscosity, viscosity arising from electron–vortex scattering, or degenerate particle viscosity will mix vortices by means of which rigid-body rotation is guaranteed for symmetric objects too. The specification of instability criteria of rapidly spinning bodies is a non-trivial point complicated issue in the framework of Einstein’s general theory of relativity. The chapter provides the derivation of the stellar structure equations in the framework of Hartle’s method.
