The chemistry of vibrationally excited H2 in the interstellar medium

TL;DR

This paper explores how vibrationally excited H2 molecules influence interstellar chemistry, especially the formation of CH+ in various astrophysical environments, using detailed chemical models.

Contribution

It provides a detailed analysis of the impact of vibrationally excited H2 reactions on interstellar molecular abundances, highlighting the conditions favoring CH+ formation.

Findings

Vibrationally excited H2 significantly enhances CH+ formation in dense, FUV-illuminated regions.

In diffuse clouds, this mechanism is insufficient to produce observed CH+ levels.

The study uses PDR models to compare different interstellar environments.

Abstract

The internal energy available in vibrationally excited H2 molecules can be used to overcome or diminish the activation barrier of various chemical reactions of interest for molecular astrophysics. In this article we investigate in detail the impact on the chemical composition of interstellar clouds of the reactions of vibrationally excited H2 with C+, He+, O, OH, and CN, based on the available chemical kinetics data. It is found that the reaction of H2 (v>0) and C+ has a profound impact on the abundances of some molecules, especially CH+, which is a direct product and is readily formed in astronomical regions with fractional abundances of vibrationally excited H2, relative to ground state H2, in excess of 10^(-6), independently of whether the gas is hot or not. The effects of these reactions on the chemical composition of the diffuse clouds zeta Oph and HD 34078, the dense PDR Orion Bar, the planetary nebula NGC 7027, and the circumstellar disk around the B9 star HD 176386 are investigated through PDR models. We find that formation of CH+ is especially favored in dense and highly FUV illuminated regions such as the Orion Bar and the planetary nebula NGC 7027, where column densities in excess of 10^(13) cm^(-2) are predicted. In diffuse clouds, however, this mechanism is found to be not efficient enough to form CH+ with a column density close to the values derived from astronomical observations.