Canonical Analysis of Radiating Atmospheres of Stars in Equilibrium

TL;DR

This paper develops a canonical framework for analyzing the radiating atmospheres of stars modeled as static, spherically symmetric spacetimes with null dust streams, facilitating their quantization.

Contribution

It introduces a canonical coordinate based on the internal time of the system, enabling linearization of the Hamiltonian constraint for quantization.

Findings

Canonical formulation of radiating star atmospheres.

Simplification of the Hamiltonian constraint.

Foundation for quantum analysis of stellar atmospheres.

Abstract

The spherically symmetric, static spacetime generated by a cross-flow of non-interacting null dust streams can be conveniently interpreted as the radiation atmosphere of a star, which also receives exterior radiation. Formally, such a superposition of sources is equivalent to an anisotropic fluid. Therefore, there is a preferred time function in the system, defined by this reference fluid. This internal time is employed as a canonical coordinate, in order to linearize the Hamiltonian constraint. This turns to be helpful in the canonical quantization of the geometry of the radiating atmosphere.