Primordial star formation: relative impact of H2 three-body rates and initial conditions

TL;DR

This study investigates how new accurate three-body H2 formation rates influence primordial star formation, revealing that their impact varies with initial conditions and halo properties, affecting thermal evolution and molecular hydrogen formation.

Contribution

The paper introduces the use of new precise three-body H2 formation rates in simulations of primordial star formation, highlighting their variable impact across different minihalos.

Findings

New rates can alter the point of full molecular hydrogen formation.

Thermal evolution varies significantly depending on initial conditions.

Correct three-body rates are as crucial as initial conditions for accurate modeling.

Abstract

Population III stars are the first stars in the Universe to form at z=20-30 out of a pure hydrogen and helium gas in minihalos of 10^5-10^6 M$_\odot$ . Cooling and fragmentation is thus regulated via molecular hydrogen. At densities above 10^8 cm$^{-3}$, the three-body H2 formation rates are particularly important for making the gas fully molecular. These rates were considered to be uncertain by at least a few orders of magnitude. We explore the impact of new accurate three-body H2 formation rates derived by Forrey (2013) for three different minihalos, and compare to the results obtained with three-body rates employed in previous studies. The calculations are performed with the cosmological hydrodynamics code ENZO (release 2.2) coupled with the chemistry package KROME (including a network for primordial chemistry), which was previously shown to be accurate in high resolution simulations. While the new rates can shift the point where the gas becomes fully molecular, leading to a different thermal evolution, there is no trivial trend in how this occurs. While one might naively expect the results to be inbetween the calculations based on Palla et al. (1983) and Abel et al. (2002), the behavior can be close to the former or the latter depending on the dark matter halo that is explored. We conclude that employing the correct three-body rates is about as equally important as the use of appropriate initial conditions, and that the resulting thermal evolution needs to be calculated for every halo individually.