Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...291..747t&link_type=abstract
Astrophysical Journal, Vol.291, NO. 2/APR15, P. 747, 1985
Astronomy and Astrophysics
Astrophysics
204
Scientific paper
We have constructed a model for the photodissociation region in Orion. This model matches the observed emission in the fine-structure lines of O I 63 μm and 145 μm, C I 609 μm, and C II 158 μ m and the low-lying rotational lines of CO. It also explains the extended H2 1-0 S(t) emission, the carbon recombination lines, and the C I 9850 Å line. The emission in the C I 370 μm, Si II 35 μm, and Fe II 26 μm, 35 μm lines is predicted. The model fit implies that a fairly uniform density (˜ 10 5 cm -3) photodissociation region lies behind the Trapezium stars. The peak temperature in this region is about 500 K, and the intensity of the incident farultraviolet (FUV) field is approximately 105 times as intense as the ambient interstellar field. This model shows that the observed high brightness temperature of the C I 609 μ m line can be explained by emission from the C+/C/CO transition region. This difference with previous chemical models is due to a higher gas phase elemental abundance of carbon, to the charge exchange reactions of C+ with S and SiO, and to carbon self-shielding.
Hollenbach David
Tielens Alexander G. G. M.
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