Barotropic thin shells with linear EOS as models of stars and circumstellar shells in general relativity

TL;DR

This paper models stars and circumstellar shells using spherically symmetric thin shells of barotropic fluids with linear equations of state in general relativity, analyzing their equilibrium and stability.

Contribution

It provides exact equations of motion, equilibrium parameters, and stability analysis for relativistic thin shell models of stars and shells.

Findings

Derived exact equations of motion for relativistic shells

Calculated equilibrium radii of static shells

Analyzed stability against radial perturbations

Abstract

The spherically symmetric thin shells of the barotropic fluids with the linear equation of state are considered within the frameworks of general relativity. We study several aspects of the shells as completely relativistic models of stars, first of all the neutron stars and white dwarfs, and circumstellar shells. The exact equations of motion of the shells are obtained. Also we calculate the parameters of the equilibrium configurations, including the radii of static shells. Finally, we study the stability of the equilibrium shells against radial perturbations.