Interstellar chemistry of nitrogen hydrides in dark clouds

Abstract

The aim of the present work is to perform a comprehensive analysis of the interstellar chemistry of nitrogen, focussing on the gas-phase formation of the smallest polyatomic species and in particular nitrogen hydrides. We present a new chemical network in which the kinetic rates of critical reactions have been updated based on recent experimental and theoretical studies, including nuclear spin branching ratios. Our network thus treats the different spin symmetries of the nitrogen hydrides self-consistently together with the ortho and para forms of molecular hydrogen. This new network is used to model the time evolution of the chemical abundances in dark cloud conditions. The steady-state results are analysed, with special emphasis on the influence of the overall amounts of carbon, oxygen, and sulphur. Our calculations are also compared with Herschel/HIFI observations of NH, NH${}_2$, and NH${}_3$ detected towards the external envelope of the protostar IRAS 16293-2422. The observed abundances and abundance ratios are reproduced for a C/O gas-phase elemental abundance ratio of $\sim 0.8$, provided that the sulphur abundance is depleted by a factor larger than 2. The ortho-to-para ratio of H${}_2$ in these models is $\sim 10^{-3}$. Our models also provide predictions for the ortho-to-para ratios of NH${}_2$ and NH${}_3$ of $\sim 2.3$ and $\sim 0.7$ respectively. We conclude that the abundances of nitrogen hydrides in dark cloud conditions are consistent with the gas-phase synthesis predicted with our new chemical network.

Accepted for publication in Astronomy & Astrophysics; 22 pages (9 in Appendix), 7 figures (2 in Appendix), 6 tables (3 in Appendix)

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