Self-gravitating anisotropic fluids. I: Context and overview

TL;DR

This paper introduces a theoretical framework for self-gravitating anisotropic fluids in Newtonian and relativistic gravity, focusing on static, spherically symmetric stellar models, and explores their structural properties and phase transitions.

Contribution

It formulates a general action-based theory for anisotropic fluids and applies it to stellar models, revealing new insights into their equilibrium and phase transition behaviors.

Findings

Anisotropic stellar models are less compact than isotropic ones.

Sequences of equilibrium configurations end at a maximum central density.

Phase transitions can prevent singularities at the stellar surface.

Abstract

This paper is the first in a sequence of three devoted to the formulation of a theory of self-gravitating anisotropic fluids in both Newtonian and relativistic gravity. In this first paper we set the stage, place our work in the context of a vast literature on anisotropic stars in general relativity, and provide an overview of the results obtained in the remaining two papers. In both cases, Newtonian and relativistic, the state of the fluid is described by the familiar variables of an isotropic fluid (such as mass density and velocity field), to which we adjoin a director vector, which defines a locally preferred direction within the fluid. Both the Newtonian and relativistic theories are defined in terms of an action functional. While each theory is formulated in complete generality, in these papers we apply them to the construction of stellar models by restricting the fluid configurations to be static and spherically symmetric. We find that the equations of anisotropic stellar structure are generically singular at the stellar surface. To avoid a singularity, we postulate the existence of a phase transition at a critical value of the mass density; the fluid is anisotropic at high densities, and goes to an isotropic phase at low densities. In the case of Newtonian stars, we find that sequences of equilibrium configurations terminate at a maximum value of the central density; beyond this maximum the density profile becomes multi-valued within the star, and the model therefore becomes unphysical. In the case of relativistic stars, this phenomenon typically occurs beyond the point at which the stellar mass achieves a maximum. Also in the case of relativistic stars, we find that for a given equation of state and a given assignment of central density, anisotropic stellar models are always less compact than isotropic models.