Fluorescent HD emission from photodissociation regions

Amiel Sternberg

doi:10.1086/169174

Fluorescent HD emission from photodissociation regions

Amiel Sternberg^*

^*Corresponding author for this work

Max-Planck-Institut für Physik und Astrophysik

Research output: Contribution to journal › Article › peer-review

7 Scopus citations

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 language	English
Pages (from-to)	121-131
Number of pages	11
Journal	Astrophysical Journal
Volume	361
Issue number	1
DOIs	https://doi.org/10.1086/169174
State	Published - 20 Sep 1990
Externally published	Yes

Keywords

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

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10.1086/169174

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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.",

keywords = "Infrared: spectra, Interstellar: molecules, Molecular processes, Nebulae: H II regions",

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N2 - 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.

AB - 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.

KW - Infrared: spectra

KW - Interstellar: molecules

KW - Molecular processes

KW - Nebulae: H II regions

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JO - Astrophysical Journal

JF - Astrophysical Journal

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Fluorescent HD emission from photodissociation regions

Abstract

Keywords

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