Abundance and chemistry of interstellar HOCO(+)

Details Abundance and chemistry of interstellar HOCO(+) Abundance and chemistry of interstellar HOCO(+)

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...244..470m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 244, no. 2, April 1991, p. 470-476.

Astronomy and Astrophysics

Astrophysics

12

Astronomical Models, Carbon Dioxide, Interstellar Matter, Magnetohydrodynamics, Molecular Ions, Astronomical Spectroscopy, Milky Way Galaxy, Photolysis, Radiative Transfer, Telescopes

Scientific paper

Column densities of 10 to the 15th/sq cm toward the Galactic center and not more than 10 to the 12th/sq cm for cold dark clouds are derived from observations using an LVG model, and the chemical implications are discussed. The HOCO(+) 4(04)-3(03) line toward Sgr A is mapped. The fractional abundance of HOCO(+) in the Galactic center region was found to be three orders of magnitude larger than predicted by quiescent ion-molecule chemistry and an order of magnitude larger than predicted by an MHD shock model. It is suggested that the possibly high CO2 abundance, and consequently the observed HOCO(+) abundance in the Galactic center, may result from UV photolysis of grain mantles.

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