On the Relation Between Interstellar H_2O and H_3O(+) Abundances

Details On the Relation Between Interstellar H_2O and H_3O(+) Abundances On the Relation Between Interstellar H_2O and H_3O(+) Abundances

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...183.1608o&link_type=abstract

American Astronomical Society, 183rd AAS Meeting, #16.08; Bulletin of the American Astronomical Society, Vol. 25, p.1316

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The interstellar chemistry of H_3O(+) is considered. It is shown that within the boundaries of the model of Phillips, van Dishoeck and Keene (1992), the abundance of H_3O(+) actually is not sensitive to the H_2O, which is inconsistent with the original conclusion of this model. Several simple relationships are derived, which express the H_3O(+) abundance as functions of the cosmic ray flux, zeta , fractional ionization, X(e), and the abundances of other chemical species. Obtained formulae are applied to the cloud L134N to specify the values of zeta , X(e), H_3 (+) abundance and so on. Derived lower limits of zeta and X(e) are 1.1 times 10(-17) s(-1) and 2.1 times 10(-8) , respectively. H_3O(+) fractional abundance ranges from 2.5 times 10({-) 9} to 1.5 times 10(-8) in this cloud.

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