Formation of Population III Stars in a flat FLRW Universe

TL;DR

This paper demonstrates that a first-order relativistic perturbation theory can explain the formation of Population III stars in a flat universe, independent of Cold Dark Matter presence, and details how mass and heat loss influence perturbation growth.

Contribution

It introduces a relativistic perturbation framework for Population III star formation in flat FLRW universes, regardless of Cold Dark Matter, highlighting the role of heat loss and particle mass.

Findings

Relativistic perturbation theory explains early star formation.

Growth rate depends on heat loss, not particle mass.

Relativistic Jeans mass varies with particle mass.

Abstract

Contrarily to general believe, a first-order cosmological perturbation theory based on Einstein's General Theory of Relativity explains the formation of massive primeval stars in a flat Friedmann-Lemaitre-Robertson-Walker universe after decoupling of matter and radiation, whether or not Cold Dark Matter is present. The growth rate of a density perturbation depends on the heat loss of a perturbation during the contraction, but is independent of the particle mass. The relativistic Jeans mass does depend on the particle mass. If the Cold Dark Matter particle mass is equal to the proton mass, then the relativistic Jeans mass is equal to 3500 solar masses, whereas the classical Jeans mass is a factor 145 larger.