Abstract
We constructed two new models for deuterium and spin-state chemistry for the purpose of modeling the low-temperature environment prevailing in starless and pre-stellar cores. The fundamental difference between the two models is in the treatment of ion-molecule proton-donation reactions of the form XH+ + Y → X + YH+, which are allowed to proceed either via full scrambling or via direct proton hop, that is, disregarding proton exchange. The choice of the reaction mechanism affects both deuterium and spin-state chemistry, and in this work our main interest is on the effect on deuterated ammonia. We applied the new models to the starless core H-MM1, where several deuterated forms of ammonia have been observed. Our investigation slightly favors the proton hop mechanism over full scrambling because the ammonia D/H ratios are better fit by the former model, although neither model can reproduce the observed NH2D ortho-to-para ratio of 3 (the models predict a value of ~2). Extending the proton hop scenario to hydrogen atom abstraction reactions yields a good agreement for the spin-state abundance ratios, but greatly overestimates the deuterium fractions of ammonia. However, one can find a reasonably good agreement with the observations with this model by increasing the cosmic-ray ionization rate over the commonly adopted value of ~ 10−17 s−1. We also find that the deuterium fractions of several other species, such as H2CO, H2O, and CH3, are sensitive to the adopted proton-donation reaction mechanism. Whether the full scrambling or proton hop mechanism dominates may be dependent on the reacting system, and new laboratory and theoretical studies for various reacting systems are needed to constrain chemical models.
Highlights
Ion-molecule proton-donation reactions are at the heart of low-temperature chemistry in the interstellar medium (ISM; Herbst & Klemperer 1973)
Our investigation slightly favors the proton hop mechanism over full scrambling because the ammonia D/H ratios are better fit by the former model, neither model can reproduce the observed NH2D ortho-to-para ratio of 3
The analysis presented above shows that neither the FS or the PH model can reproduce the NH2D o/p abundance ratio observed toward H-MM1 regardless of variations in the physical core model, and that the various modeled D/H ratios differ from the observed values
Summary
Ion-molecule proton-donation reactions are at the heart of low-temperature chemistry in the interstellar medium (ISM; Herbst & Klemperer 1973). Spin-state and deuterium chemistry are very closely tied, and to understand observations of deuterated species through chemical modeling, one needs to take spin-state chemistry into consideration. Several such chemical models have been introduced in the past decades, describing gasphase or gas-grain chemistry (e.g., Pagani et al 1992; Walmsley et al 2004; Sipilä et al 2010; Furuya et al 2015; Roueff et al 2015; Hily-Blant et al 2018). In this paper we investigate the effect of proton exchange on ion-molecule chemistry in the ISM by modifying the chemical model of Sipilä et al (2015), allowing proton-donation reactions, in which proton exchanges were previously allowed, to proceed instead through PH only.
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