Amending the computation of the mass of compact rotating bodies with non-zero energy density at the surface.
A proper understanding of rotating bodies in General Relativity (GR) is fundamental for many astrophysical situations. The original relativistic treatment of rotating compact stars in equilibrium is due to Hartle, back in 1967. It constitutes the basis of most of the analytical approaches and is widely used to construct numerical schemes in axial symmetry.
Hartle’s scheme depicts the equilibrium (stationary regime) Continue reading