A model for the intense molecular line emission from OMC-1

Details A model for the intense molecular line emission from OMC-1 A model for the intense molecular line emission from OMC-1

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...259l..91d&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 259, Aug. 15, 1982, p. L91-L96.

Astronomy and Astrophysics

Astronomy

142

Astronomical Models, Interstellar Gas, Interstellar Magnetic Fields, Magnetohydrodynamic Waves, Orion Nebula, Shock Waves, Carbon Monoxide, Hydrogen, Infrared Spectra, Line Spectra, Radio Astronomy

Scientific paper

A model is presented which attributes the observed H2 and CO line emission from OMC-1 to a magnetohydrodynamic shock propagating into magnetized molecular gas. By requiring the shock to reproduce the observed line intensities, the shock speed is determined to be approximately 38 km/s and the preshock density and (transverse) magnetic field to be 700,000 per cu cm and 1.5 milligauss. The model is compared to observations of H2, CO, OH, O I, and C I in emission and of CO in absorption. The shocked gas may be detectable in H I 21 cm emission.

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