Modelling the chemical evolution of molecular clouds as a function of metallicity
arXiv:1403.0765 · doi:10.1093/mnras/stu207
Abstract
The Galaxy is in continuous elemental evolution. Since new elements produced by dying stars are delivered to the interstellar medium, the formation of new enerations of stars and planetary systems is influenced by this metal enrichment. We aim to study the role of the metallicity on the gas phase chemistry of the interstellar medium. Using a system of coupled-ordinary differential equations to model the chemical reactions, we simulate the evolution of the abundance of molecules in the gas phase for different initial interstellar elemental compositions. These varying initial elemental compositions consider the change in the "elemental abundances" predicted by a self-consistent model of the elemental evolution of the Galaxy. As far as we are aware, this is the first attempt to combine elemental evolution of the Galaxy and chemical evolution of molecular clouds. The metallicity was found to have a strong effect on the overall gas phase composition. With decreasing metallicity, the number of long carbon chains was found to increase, the time-scale on which small molecular species are increases, and the main form of oxygen changed from O and CO to O2. These effects were found to be mainly due to the change in electron, H3+, and atomic oxygen abundance.
15 figures 4 tables. Monthly Notices of the Royal Astronomical Society 2014
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