Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...224..448b&link_type=abstract
Astrophysical Journal, Part 1, vol. 224, Sept. 1, 1978, p. 448-452.
Astronomy and Astrophysics
Astrophysics
66
Abundance, Hydrogen Clouds, Interstellar Chemistry, Nebulae, Astronomical Models, Calcium, Electron Density (Concentration), Ionization, Photodissociation, Sodium, Ultraviolet Radiation
Scientific paper
A model of the interstellar cloud lying along the line of sight to Zeta Persei is constructed using procedures based on the hypotheses that H2 is formed on grain surfaces and destroyed by UV fluorescence, that the populations of low-lying rotational levels of H2 are characterized by the ambient kinetic temperature, and that the populations of high-lying rotational levels are determined by UV pumping and the grain formation process. The gas-phase reaction scheme includes the radiative association C(+) + H2 yields CH2(+) + a photon and the charge transfer H(+) + O yields H + O(+). The model cloud structure consists of a core with a total hydrogen density of 267 per cu cm and a temperature of 45 K surrounded by an envelope with a density of 100 per cu cm and a temperature of 120 K. It is shown that this model reproduces the ionization structure of Na, Si, K, and Ca, predicts abundances of the molecules OH, CO, CN, and CH in satisfactory agreement with observations, but underestimates the abundance of CH(+) by a factor of 4.
Black John Harry
Dalgarno Alexander
Hartquist Thomas W.
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