Surface chemistry in the Interstellar Medium II. $\mathrm{H}_2$ formation on dust with random temperature fluctuations

TL;DR

This study investigates how simultaneous dust temperature and surface hydrogen atom fluctuations influence molecular hydrogen formation on interstellar dust grains, revealing that fluctuations significantly affect formation rates and observable emissions.

Contribution

It extends the master equation approach to coupled fluctuations, providing new insights into H2 formation mechanisms under realistic astrophysical conditions.

Findings

Langmuir-Hinshelwood mechanism becomes efficient in PDR edges with fluctuations

Fluctuations can reduce formation efficiency in cloud cores

Simpler rate equations are adequate for most observational interpretations

Abstract

The $\mathrm{H}_2$ formation on grains is known to be sensitive to dust temperature, which is also known to fluctuate for small grain sizes due to photon absorption. We aim at exploring the consequences of simultaneous fluctuations of the dust temperature and the adsorbed H-atom population on the $\mathrm{H}_2$ formation rate under the full range of astrophysically relevant UV intensities and gas conditions. The master equation approach is generalized to coupled fluctuations in both the grain's temperature and its surface population and solved numerically. The resolution can be simplified in the case of the Eley-Rideal mechanism, allowing a fast computation. For the Langmuir-Hinshelwood mechanism, it remains computationally expensive, and accurate approximations are constructed. We find the Langmuir-Hinshelwood mechanism to become an efficient formation mechanism in unshielded photon dominated region (PDR) edge conditions when taking those fluctuations into account, despite hot average dust temperatures. It reaches an importance comparable to the Eley-Rideal mechanism. However, we show that a simpler rate equation treatment gives qualitatively correct observable results in full cloud simulations under most astrophysically relevant conditions. Typical differences are a factor of 2-3 on the intensities of the $\mathrm{H}_2$ $v=0$ lines. We also find that rare fluctuations in cloud cores are sufficient to significantly reduce the formation efficiency. Our detailed analysis confirms that the usual approximations used in numerical models are adequate when interpreting observations, but a more sophisticated statistical analysis is required if one is interested in the details of surface processes.