Chemical model calculations of C2, C3, CH, CN, OH, and NH2 abundances in cometary comae

Details Chemical model calculations of C2, C3, CH, CN, OH, and NH2 abundances in cometary comae Chemical model calculations of C2, C3, CH, CN, OH, and NH2 abundances in cometary comae

Mar 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...244.1087m&link_type=abstract

Astrophysical Journal, Part 1, vol. 244, Mar. 15, 1981, p. 1087-1093. Research supported by the Natural Sciences and Engineerin

Astronomy and Astrophysics

Astrophysics

48

Abundance, Carbon, Chemical Reactions, Comets, Hydrocarbons, Molecular Interactions, Ammonia, Astronomical Models, Chemical Composition, Comet Nuclei, Cyanides, Hydroxyl Radicals, Interstellar Matter

Scientific paper

One-dimensional radial models of the chemistry in cometary comae have been constructed using a comprehensive system of chemical reactions for a number of assumed nuclear compositions. Column abundances for C2, C3, CR, OH, CN, and NH2 calculated from these models are compared to those calculated from observations. Models which assume a parent volatile mixture consisting of the simplest species containing carbon, oxygen, and nitrogen -- H2O, CO2, CR4, and NH3 -produce column abundances of C2, OH, CR, and NH2 consistent with observations but do not produce sufficient amounts of C3 and CN. Models which assume a more complex mixture of parent volatiles, derived by assuming comets originate from a gas with composition similar to that found in interstellar molecular clouds, are successful in accounting for the observed coma column abundances of C2, C3, CN, CR, OH, and NH2.

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