Molecular and thermal equilibrium in low density interstellar clouds. II - Model predictions

Details Molecular and thermal equilibrium in low density interstellar clouds. II - Model predictions Molecular and thermal equilibrium in low density interstellar clouds. II - Model predictions

Jan 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....54..345b&link_type=abstract

Astronomy and Astrophysics, vol. 54, no. 2, Jan. 1977, p. 345-354. Research supported by the Deutsche Forschungsgemeinschaft.

Astronomy and Astrophysics

Astrophysics

38

Abundance, Chemical Equilibrium, Interstellar Matter, Plasma Clouds, Thermodynamic Equilibrium, Carbon Monoxide, Electron Clouds, Electron Density (Concentration), Hydrogen Clouds, Hydroxyl Radicals, Space Density, Water Vapor

Scientific paper

Chemical and thermal equilibrium in interstellar clouds with low optical depths and electron densities of 10 to 10,000 per cu cm is examined by analyzing a model for the center of a chemically and physically homogeneous spherical molecular cloud. Cloud temperatures are determined by computing the ortho-to-para hydrogen abundance ratio, possible heating mechanisms are considered, and equilibrium temperatures are derived for clouds with both solar and depleted abundances. H2 and H(+) concentrations as well as HD/H2 ratios are calculated as a function of density and oxygen abundance for two cosmic-ray ionization rates, and reactions are analyzed which involve CO, OH, H2O, O2, NO, and N2. CH, CH(+), and CN abundances are predicted as a function of density and compared with observations. It is concluded that temperatures corresponding to those observed (greater than 50 K) are impossible at electron densities higher than 100 per cu cm without considerable depletion of carbon.

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