Predictions of line intensities from hydrostatic models of molecular clouds

Details Predictions of line intensities from hydrostatic models of molecular clouds Predictions of line intensities from hydrostatic models of molecular clouds

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982esasp.189..115b&link_type=abstract

In ESA The Sci. Importance of Submillimetre Observations p 115-117 (SEE N83-22034 11-88)

Astronomy and Astrophysics

Astronomy

Astronomical Models, Brightness Temperature, Carbon, Line Spectra, Molecular Clouds, Submillimeter Waves, Cosmic Rays, Hydrogen, Ionizing Radiation, Photoelectrons, Physical Properties, Radio Astronomy

Scientific paper

Plane parallel and spherical models of cold dense molecular clouds were constructed. The gas is heated predominantly by photoelectrons from dust grains in the outer parts of the clouds and by cosmic ray ionizations of molecular hydrogen in the inner parts. It is cooled by fine structure excitation followed by radiative decay of C+ ions and c atoms in the outer parts of the clouds and by rotational excitation of CO molecules followed by radiative decay in the inner parts. The brightness temperatures of several millimeter and submillimeter lines of C+, C, CO and HCO for our spherical cloud models are calculated. Observations in the directions of L134 and L183 are compared.

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