Existence and uniqueness of compact rotating configurations in GR in second order perturbation theory

TL;DR

This paper proves the existence and uniqueness of slowly rotating fluid bodies in equilibrium within General Relativity using second order perturbation theory, clarifying the structure of such configurations in the strong field regime.

Contribution

It derives the Hartle-Thorne model from first principles for rigidly rotating perfect fluid balls, establishing conditions for existence and uniqueness in second order perturbation theory.

Findings

Spacetime is equatorially symmetric at this approximation level.

Configurations are fully determined by central pressure and angular velocity.

The model is derived with minimal assumptions on perturbation regularity.

Abstract

Existence and uniqueness of rotating fluid bodies in equilibrium is still poorly understood in General Relativity (GR). Apart from the limiting case of infinitely thin disks, the only known global results in the stationary rotating case (Heilig [14] and Makino [21] [arXiv:1705.07392]) show existence in GR nearby a Newtonian configuration (under suitable additional restrictions). In this work we prove existence and uniqueness of rigidly (slowly) rotating fluid bodies in equilibrium to second order in perturbation theory in GR. The most widely used perturbation framework to describe slowly rigidly rotating stars in the strong field regime is the Hartle-Thorne model. The model involves a number of hypotheses, some explicit, like equatorial symmetry or that the perturbation parameter is proportional to the rotation, but some implicit, particularly on the structure and regularity of the perturbation tensors and the conditions of their matching at the surface. In this work, with basis on the gauge results obtained in [25], the Hartle-Thorne model is fully derived from first principles and only assuming that the perturbations describe a rigidly rotating finite perfect fluid ball (with no layer at the surface) with the same barotropic equation of state as the static ball. Rigidly rotating fluid balls are analyzed consistently in second order perturbation theory by imposing only basic differentiability requirements and boundedness. Our results prove in particular that, at this level of approximation, the spacetime must be indeed equatorially symmetric and is fully determined by two parameters, namely the central pressure and the uniform angular velocity of the fluid.