Stability of Polytropes

TL;DR

This paper studies the stability of ideal star models called polytropes within General Relativity, focusing on boundary conditions and the stability of various configurations, including double polytropes with infinite atmospheres.

Contribution

It introduces a revised boundary condition approach and analyzes the stability of double polytropes with variable indices, extending understanding of star stability in strong gravitational fields.

Findings

All static configurations are stable.

Confirmed mass-radius relation and upper mass limit.

Investigated double polytropes with infinite atmospheres.

Abstract

This paper is an investigation of the stability of some ideal stars. It is in- tended as a study in General Relativity, with emphasis on the coupling to matter, eventually aimed at a better understanding of very strong gravitational fields and Black Holes. The work is based on an action principle for the complete system of metric and matter fields. We propose a complete revision of the treatment of boundary conditions. An ideal star in our terminology has spherical symmetry and an isentropic equation of state. In our first work on this subject it was assumed that the density vanishes beyond a finite distance from the origin. But it is difficult to decide what the proper boundary conditions should be and we are consequently skeptical of the concept of a fixed boundary. In this paper we investigate the double polytrope, characterized by a polytropic index n less than 5 in the bulk of the star and a value larger than 5 in an outer atmosphere that extends to infinity. It has no fixed boundary but a region of critical density where the polytropic index changes from a value that is appropriate for the bulk of the star to a value that provides a crude model for the atmosphere. The existence of a relation between mass and radius is confirmed, as well as an upper limit on the mass. The principal conclusion is that all the static configurations are stable.