Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...259..271g&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 259, no. 1, p. 271-282.
Astronomy and Astrophysics
Astronomy
60
Carbon Monoxide, Far Ultraviolet Radiation, Interstellar Matter, Molecular Clouds, Ultraviolet Astronomy, Line Spectra, Radiative Transfer
Scientific paper
We have performed CO line radiative transfer computations for spherically symmetric clumps that are irradiated by FUV radiation of intermediate strength. The clumps are assumed to have sizes of about 1 pc, a radially varying density, and a temperature and chemical distribution, including fractionation of (C-12)O and (C-13)O, according to photodissociation region (PDR) models. The model reproduces successfully the (C-12)O and (C-13)O J = 1 - 0 and J = 2 - 1 intensities observed in the Orion A molecular cloud and other sources that cannot be accounted for in simple single-component radiative transfer calculations. The (C-12)O lines are shown to emerge from the roughly 30 K warm layer at the bottom of the PDR, whereas the (C-13)O lines exhibit additionally a substantial contribution from the cold isothermal clump core. Different beam-filling of the (C-12)O and (C-13)O lines plays a minor role for the intensity ratios.
Gierens Klaus M.
Stutzki Juergen
Winnewisser Gisbert
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