Physical conditions of the Orion Nebula derived from optical and ultraviolet data

Details Physical conditions of the Orion Nebula derived from optical and ultraviolet data Physical conditions of the Orion Nebula derived from optical and ultraviolet data

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982nyasa.395...24p&link_type=abstract

(NASA, National Science Foundation, New York Academy of Sciences, et al., Symposium on the Orion Nebula to Honor Henry Draper, N

Astronomy and Astrophysics

Astronomy

27

Interstellar Gas, Molecular Clouds, Orion Nebula, Abundance, Astronomical Models, Chemical Composition, Gas Flow, H Ii Regions, Temperature Distribution, Ultraviolet Spectra

Scientific paper

The structure and chemical composition of the Orion Nebula is reviewed. The velocity and pressure patterns of the core region are more complex than those predicted by models in which the gas flow originates in the molecular cloud. There is an H II region around θ2 Ori that is disconnected from the main H II region produced by the Trapezium. The emission lines from the outer regions (r ⪆ 12arcmin) are mainly produced by dust-scattered light, i.e., the outer shell is a reflection nebula and not an H II region. The gaseous abundances of C, N, O, Ne, and S relative to H are 0.2±0.2 dex smaller than those in the Sun.

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