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The photodissociation and chemistry of interstellar CO
Open accessAbstract
Recent work on the vacuum ultraviolet absorption spectrum of CO by Letzelter et al. and Yoshino et al. has clarified the nature of its photodissociation processes. The application of these spectroscopic data to the description of the photodissociation of interstellar CO and its principal isotopic varieties 13CO, C18O, and 13C18O is discussed. The unattenuated photodissociation rate of interstellar CO is ≡2 × 10-10s-1, more than an order of magnitude larger than the value used in previous models. The new treatment of the CO photodissociation has been incorporated into detailed models of the structure and chemistry of interstellar clouds. Computed abundances of CO and related species C and C+ are presented for a variety of interstellar clouds ranging from diffuse clouds to dense photodissociation regions. The model results are compared with a variety of observational data on both the CO and C abundances in such clouds.
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Citations
Cited by
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“However, molecular clouds are surrounded by atomic envelopes and a transition region in which the hydrogen is primarily molecular, but the carbon is mostly atomic (van Dishoeck & Black 1988).”
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“For the dust absorption term fdust,CO, we use the expression (van Dishoeck & Black 1988) fdust,CO = exp (−2.5AV) (21) using the same relationship as before between the visual extinction AV and the total hydrogen column density NH,tot.”
BackgroundMethodInfluential
Metadata
- Authors
- van Dishoeck, E. F., & Black, J. H.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 1988-11
- Volume
- 334
- Pages
- 771
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2032832347
- Cited by
- 943
- References
- 0
- FWCI
- 18.11
- Type
- journal article
- Language
- en
- Open access
- bronze
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