Rydberg States of H$_3$ and HeH as Potential Coolants for Primordial Star Formation

TL;DR

This paper explores the potential of Rydberg states of H$_3$ and HeH as cooling agents in primordial star formation, reviewing recent spectroscopic observations and proposing new ideas for understanding early universe gas cooling mechanisms.

Contribution

It introduces the idea that Rydberg states of H$_3$ and HeH could serve as novel coolants in primordial star formation, supported by recent spectroscopic data.

Findings

Spectroscopic observations of H$_3$ Rydberg states in the mid-infrared.

Proposed new mechanisms for primordial gas cooling involving Rydberg states.

Discussion of how these states could influence early star formation processes.

Abstract

Current theory and measurements establish the age of the universe as ca. 13.8 billion years. For the first several hundred million years of its existence, it was a dark, opaque void. After that, the hydrogen atoms comprising most of the "ordinary" matter began to condense and ionize, eventually forming the first stars that would illuminate the sky. Details of how these "primordial" stars formed have been widely debated, but remain elusive. A central issue in this process is the mechanism by which the primordial gas (mainly hydrogen and helium atoms) collected via the action of dark matter cools and further accretes to fusion densities. Current models invoke collisional excitation of H$_2$ molecular rotations and subsequent radiative rotational transitions allowed by the weak molecular quadrupole moment. In this article, we review the salient considerations, and present some new ideas, bases on recent spectroscopic observations of neutral H$_3$ Rydberg electronic state emission in the mid-infrared.