The abundance of H3(+) ions in dense interstellar clouds

Details The abundance of H3(+) ions in dense interstellar clouds The abundance of H3(+) ions in dense interstellar clouds

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...321..383l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 321, Oct. 1, 1987, p. 383-385.

Statistics

Computation

30

Abundance, Cosmic Rays, Gas Density, Hydrogen Ions, Ion Production Rates, Molecular Clouds, Computational Astrophysics, Hydroxyl Emission, Interstellar Chemistry, Interstellar Matter, Photodissociation

Scientific paper

Several simple relationships are written down which express the abundances of C+, He+, H3+, OH, and H2O in dense interstellar clouds as functions of the cosmic-ray ionization rate. It is argued that the primary source of OH is photodissociation of H2O by cosmic-ray induced photons. The abundance of H3+ is derived from observations of OH and predicted to be typically about 2 x 10-5 cm-3, independent of density. Lower limits of respectively 4 x 10-18 s-1 and 8 x 10-18 s-1 are obtained for the cosmic-ray ionization rates in the clouds L134 and B335. The abundances of H3+ are likely to be enhanced in regions in which the DCO+/HCO+ ratio is large.

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