Spherical Isentropic Protostars in General Relativity

TL;DR

This paper derives and analyzes interior solutions to Einstein's equations for spherical, isentropic gas clouds in general relativity, exploring their structure and potential implications for star formation and gamma-ray burst phenomena.

Contribution

It introduces a novel approach to modeling isentropic protostars within general relativity, providing analytic and numerical solutions for their mass and metric structures.

Findings

Solutions indicate the presence of shell-like mass distributions.

Analytic and numerical models of isentropic gas structures are developed.

Potential relevance to solar system formation and gamma-ray burst ejections.

Abstract

In the process of protostar formation, astrophysical gas clouds undergo thermodynamically irreversible processes and emit heat and radiation to their surroundings. Due the emission of this energy one can envision an idealized situation in which the gas entropy remains nearly constant. In this setting, we derive in this paper interior solutions to the Einstein equations of General Relativity for spheres which consist of isentropic gas. To accomplish this objective we derive a single equation for the cumulative mass distribution in the protostar. From a solution of this equation one can infer readily the coefficients of the metric tensor. In this paper we present analytic and numerical solutions for the structure of the isentropic self-gravitating gas. In particular we look for solutions in which the mass distribution indicates the presence of shells, a possible precursor to solar system formation. Another possible physical motivation for this research comes from the observation that gamma ray bursts are accompanied by the ejection of large amounts of thermodynamically active gas at relativistic velocities. Under these conditions it is natural to use the equations of general relativity to inquire about the structure of the ejected mass.