Editing Ammonia (section)

==== Interstellar destruction mechanisms ====
There are 113 total proposed reactions leading to the destruction of {{chem2|NH3}}. Of these, 39 were tabulated in extensive tables of the chemistry among C, N and O compounds.<ref>{{cite journal|bibcode=1980ApJS...43....1P|author1=Prasad, S. S. |author2=Huntress, W. T. |title=A model for gas phase chemistry in interstellar clouds|year=1980|journal=The Astrophysical Journal Supplement Series |volume=43|page=1 | doi=10.1086/190665|doi-access=free}}</ref> A review of interstellar ammonia cites the following reactions as the principal dissociation mechanisms:<ref name="Ho-1983"/>

{{NumBlk|:| {{chem2|NH3 + [H3]+ → [NH4]+ + H2}}|{{EquationRef|1}}}}
{{NumBlk|:| {{chem2|NH3 + HCO+ → [NH4]+ + CO}}|{{EquationRef|2}}}}

with rate constants of 4.39×10<sup>−9</sup><ref>{{cite journal|author1=Lininger, W. |author2=Albritton, D. L. |author3=Fehsenfeld, F. C. |author4=Schmeltekopf, A. L. |author5=Ferguson, E. E. |journal= J. Chem. Phys.|volume=62|page=3549|year=1975|bibcode = 1975JChPh..62.3549L |doi = 10.1063/1.430946|title=Flow–drift tube measurements of kinetic energy dependences of some exothermic proton transfer rate constants|issue=9 }}</ref> and 2.2×10<sup>−9</sup>,<ref>{{cite journal|doi=10.1016/0009-2614(77)85326-8|title=Reactions of CH<sup>+</sup><sub>n</sub> IONS with ammonia at 300&nbsp;K|year=1977|author=Smith, D.|journal=Chemical Physics Letters|volume=47|issue=1|page=145|first2=N. G.|last2=Adams|bibcode = 1977CPL....47..145S }}</ref> respectively. The above equations ({{EquationNote|1}}, {{EquationNote|2}}) run at a rate of 8.8×10<sup>−9</sup> and 4.4×10<sup>−13</sup>, respectively. These calculations assumed the given rate constants and abundances of [{{chem2|NH3}}]/[{{chem2|H2}}] = 10<sup>−5</sup>, [{{chem2|[H3]+}}]/[{{chem2|H2}}] = 2×10<sup>−5</sup>, [{{chem2|HCO+}}]/[{{chem2|H2}}] = 2×10<sup>−9</sup>, and total densities of ''n'' = 10<sup>5</sup>, typical of cold, dense, molecular clouds.<ref>{{cite journal|author1=Wooten, A. |author2=Bozyan, E. P. |author3=Garrett, D. B. |year=1980|journal=Astrophysical Journal|title=Detection of C<sub>2</sub>H in cold dark clouds|bibcode=1980ApJ...239..844W|volume=239|page=844|doi=10.1086/158168}}</ref> Clearly, between these two primary reactions, equation ({{EquationNote|1}}) is the dominant destruction reaction, with a rate ≈10,000 times faster than equation ({{EquationNote|2}}). This is due to the relatively high abundance of {{chem2|[H3]+}}.