Rate of three-body recombination of hydrogen molecules during primordial star formation

TL;DR

This paper provides a new, more reliable calculation of the three-body recombination rate of hydrogen molecules during primordial star formation, addressing significant discrepancies in existing data.

Contribution

It offers an independent calculation and an analytic expression for the recombination rate, improving the accuracy of astrophysical models of primordial star formation.

Findings

New analytic expression for recombination rate

Addresses discrepancies in existing rate constants

Enhances reliability of primordial star formation models

Abstract

Astrophysical models of primordial star formation require rate constants for three-body recombination as input. The current status of these rates for H2 due to collisions with H is far from satisfactory, with published rate constants showing orders of magnitude disagreement at the temperatures relevant for H2 formation in primordial gas. This letter presents an independent calculation of this recombination rate constant as a function of temperature. An analytic expression is provided for the rate constant which should be more reliable than ones currently being used in astrophysical models.