Metallic species in interstellar medium: Astrochemical modeling

Abstract

Metal-bearing species in diffuse or molecular clouds are often overlooked in astrochemical modeling except for the charge exchange process. However, catalytic cycles involving these metals can affect the abundance of other compounds. We prepared a comprehensive chemical network for Na, Mg, Al, Fe, K, and Si-containing species. Assuming water as the major constituent of interstellar ice in dark clouds, quantum chemical calculations were carried out to estimate the binding energy of important metallic species, considering amorphous solid water as substrate. Significantly lower binding energies (approximately 5 to 6 times) were observed for Na and Mg, while the value for Fe was roughly 4 times higher than what was used previously. Here, we calculated binding energy values for Al and K, for which no prior guesses were available. The total dipole moments and enthalpies of formation for several newly included species are unknown. Furthermore, the assessment of reaction enthalpies is necessary to evaluate the feasibility of the new reactions under interstellar conditions. These parameters were estimated and subsequently integrated into models. Some additional species that were not included in the UMIST/KIDA database have been introduced. The addition of these new species, along with their corresponding reactions, appears to significantly affect the abundances of related species. Some key reactions that significantly influence general metal-related chemistry include: ${\mathrm{M}}^{+}+{\mathrm{H}}_2\to \mathrm{M}{{\mathrm{H}}_2}^{+}+\mathrm{h}\nu$, $\mathrm{MH}+\mathrm{O}\to \mathrm{MO}+\mathrm{H}$ ($\mathrm{M}=\mathrm{Fe},\mathrm{Na},\mathrm{Mg},\mathrm{Al},\mathrm{K}$), and ${\mathrm{M}}_1^{+}+{\mathrm{M}}_2\mathrm{H}\to {\mathrm{M}}_1\mathrm{H}+{\mathrm{M}}_2^{+}$ (where ${\mathrm{M}}_1\ne {\mathrm{M}}_2$, $M_1,M_2=Na,Mg,Al,K,Fe$). Significant changes were observed in magnesium and sodium-bearing cyanides, isocyanides, and aluminum fluoride when additional reaction pathways were considered.

16 pages, 6 figures, Accepted for publication in Astronomy and Astrophysics

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