Complexity and white-dwarf structure

TL;DR

This paper investigates how the complexity measure of white dwarf stars varies from low-mass to relativistic regimes, showing it increases with mass and peaks at the Chandrasekhar limit.

Contribution

It introduces a novel application of complexity measures to stellar density profiles, extending previous atomic studies to astrophysical objects.

Findings

Complexity increases with white dwarf mass.

Maximum complexity occurs at the Chandrasekhar limit.

Complexity reaches a finite maximum in the relativistic regime.

Abstract

From the low-mass non-relativistic case to the relativistic limit, the density profile of a white dwarf is used to evaluate the complexity measure. Similarly to the recently reported atomic case where, by averaging shell effects, complexity grows with the atomic number, here complexity grows as a function of the star mass reaching a maximum finite value in the Chandrasekhar limit.