Abstract
Computations are presented of the IR fluorescent HD emission spectrum that is produced in cold isothermal static photodissociation regions at the surfaces of interstellar molecular clouds exposed to UV radiation. A scaling equation is derived which relates the HD line intensities to the gas density, the intensity of the incident UV radiation, the grain-surface molecular-formation rate coefficient, and the cosmic-ray ionization rate. Fluorescent HD emission lines may be detectable from dense photodissociation regions with hydrogen densities equal to about 5 x 10 to the 6th/cu cm which are exposed to intense UV fields. 36 refs.
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