Fluorescent HD emission from photodissociation regions

Research output: Contribution to journalArticlepeer-review

Abstract

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 ultraviolet (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 ∼5 x 106 cm-3 which are exposed to intense UV fields.

Original languageEnglish
Pages (from-to)121-131
Number of pages11
JournalAstrophysical Journal
Volume361
Issue number1
DOIs
StatePublished - 20 Sep 1990
Externally publishedYes

Keywords

  • Infrared: spectra
  • Interstellar: molecules
  • Molecular processes
  • Nebulae: H II regions

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