Fluorescent HD emission from photodissociation regions

Details Fluorescent HD emission from photodissociation regions Fluorescent HD emission from photodissociation regions

Mar 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990stin...9119982s&link_type=abstract

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D Lines, H Lines, Infrared Spectra, Interstellar Matter, Molecular Clouds, Photodissociation, Emission Spectra, Extreme Ultraviolet Radiation, Line Spectra

Scientific paper

Computations are presented of the infrared 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 approximately 5,000,000/cu cm which are exposed to intense UV fields.

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