![]() ![]() Furthermore, the study of the tautomerization of HNC to HCN (and vice versa), which has been studied extensively, has been suggested as a model by which more complicated isomerization reactions can be studied. This makes the study of the reaction pathways that lead to its formation and destruction a good means of obtaining insight to the workings of these reactions in space. Aside from having its J = 1→0 transition in a clear portion of the atmospheric window, as well as having numerous isotopomers also available for easy study, and in addition to having a large dipole moment that makes observations particularly simple, HNC is, in its molecular nature, a quite simple molecule. ![]() The study of HNC is a relatively simple pursuit, and this is one of the greatest motivations for its study. Furthermore, the HNC/HCN line ratio is used to distinguish between photodissociation regions and X-ray-dissociation regions on the basis that / is roughly unity in the former, but greater than unity in the latter. This information provides great insight into the mechanisms of the formation of (Ultra-)Luminous Infrared Galaxies ((U)LIRGs), as it provides data on the nuclear environment, star formation, and even black hole fueling. The HCO +/HNC line ratio is used to good effect as a measure of density of gas. Aside from the potential to use HNC to investigate gravitational collapse as the means of star formation, HNC abundance (relative to the abundance of other nitrogenous molecules) can be used to determine the evolutionary stage of protostellar cores. As such, an understanding of the chemistry of HNC leads to an understanding of countless other species-HNC is an integral piece in the complex puzzle representing interstellar chemistry.įurthermore, HNC (alongside HCN) is a commonly used tracer of dense gas in molecular clouds. HNC is intricately linked to the formation and destruction of numerous other molecules of importance in the interstellar medium-aside from the obvious partners HCN, protonated hydrogen cyanide (HCNH +), and cyanide (CN), HNC is linked to the abundances of many other compounds, either directly or through a few degrees of separation. Many other related species (including HCN) are observed in roughly the same window. This transition occurs at ~90.66 GHz, which is a point of good visibility in the atmospheric window, thus making astronomical observations of HNC particularly simple. In practice, HNC is almost exclusively observed astronomically using the J = 1→0 transition. ![]() This is because of the potential energy path of the tautomerization reaction there is an activation barrier on the order of roughly 12,000 cm −1 for the tautomerization to occur, which corresponds to a temperature at which HNC would already have been destroyed by neutral-neutral reactions. These large dipole moments facilitate the easy observation of these species in the interstellar medium.Īs HNC is higher in energy than HCN by 3920 cm −1 (46.9 kJ/mol), one might assume that the two would have an equilibrium ratio ( ) e q is much higher than 10 −25, and is in fact on the order of unity in cold environments. Both HNC and HCN have large, similar dipole moments, with μ HNC = 3.05 Debye and μ HCN = 2.98 Debye respectively. It is a zwitterion and an isomer of hydrogen cyanide (HCN). Hydrogen isocyanide (HNC) is a linear triatomic molecule with C ∞v point group symmetry. The second one is according to the substitutive nomenclature rules, derived from the parent hydride azane ( NH 3) and the anion methanide ( CH − 3). Its importance in the field of astrochemistry is linked to its ubiquity in the interstellar medium.īoth hydrogen isocyanide and azanylidyniummethanide are correct IUPAC names for HNC. It is a minor tautomer of hydrogen cyanide (HCN). Hydrogen isocyanide is a chemical with the molecular formula HNC. ![]()
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