Searches for the protonated interstellar species HC3NH(+), CH3CNH(+), and HOCS(+) - Implications for ion-molecule chemistry

Details Searches for the protonated interstellar species HC3NH(+), CH3CNH(+), and HOCS(+) - Implications for ion-molecule chemistry Searches for the protonated interstellar species HC3NH(+), CH3CNH(+), and HOCS(+) - Implications for ion-molecule chemistry

Jan 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...349..376t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 349, Jan. 20, 1990, p. 376-387.

Astronomy and Astrophysics

Astrophysics

18

Electron Recombination, Interstellar Chemistry, Molecular Ions, Positive Ions, Astronomical Models, Gas-Ion Interactions, Interstellar Matter, Molecular Clouds, Molecular Interactions

Scientific paper

It is reported here that observed limits for the interstellar abundance ratios HC3NH(+)/HC3N, CH3CNH(+)/CH3CN, and HOCS(+)/OCS are consistent with current interstellar ion-molecule formation models, although the low abundance of HC3NH(+) precludes several reaction pathways for forming higher-order cyanopolyynes. It is also reported that HC3NH(+)/HC3N is at least 10 times smaller than HCNH(+)/CHN, a result that is not explainable solely by ion-molecule processes and that may suggest a non-gas-phase depletion mechanism for HCN such as absorption onto grains. There is no evidence for high-temperature HOCS(+)/OCS chemistry.

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