Slowly-rotating cosmological perfect fluids
The Einstein field equations for a perfect fluid distribution representing slowly-rotating fluid spheres are investigated. By imposing restrictions on the matter rotation \(\omega\) (r,t) which is related to the dragging of inertial frames, and a uniform rotation which is a function of time, the general solutions for \(\Omega\) (r,t) are obtained for all cosmological models. In the case of closed models the solutions for \(\Omega\) (r,t) may represent realistic astrophysical situations only when the radial distance is greater than -1 and less than \(+1\).
scientific article; zbMATH DE number 4025095