Can interstellar H2S be formed via gas-phase reactions? - Calculations concerning the rates of the ternary and radiative association reactions between HS(+) and H2

Details Can interstellar H2S be formed via gas-phase reactions? - Calculations concerning the rates of the ternary and radiative association reactions between HS(+) and H2 Can interstellar H2S be formed via gas-phase reactions? - Calculations concerning the rates of the ternary and radiative association reactions between HS(+) and H2

Apr 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989mnras.237.1057h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 237, April 15, 1989, p. 1057-1065.

Mathematics

Probability

22

Hydrogen Sulfide, Interstellar Chemistry, Interstellar Gas, Abundance, Association Reactions, Hydrogen, Molecular Ions, Orion Nebula, Reaction Kinetics

Scientific paper

Based on laboratory work involving the ternary association reaction of HS+ and H2 at 80 K, we have estimated the rate of the analogous radiative association reaction under interstellar conditions. Both the ternary and radiative association reactions appear to occur via a mechanism in which the electronic spin of the H3S+ complex changes before the complex is stabilized. Although this spin change is of low probability, it leads to a radiative association rate coefficient at 80 K of 7 × 10-16 cm3 s-1 if radiative stabilization occurs at a rate of 103 s-1. This value of the radiative association rate coefficient at 80 K is large enough to lead to the observed abundance of H2S in the ambient ridge source in Orion.

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