The source of high-velocity emission at the Orion molecular cloud core

Details The source of high-velocity emission at the Orion molecular cloud core The source of high-velocity emission at the Orion molecular cloud core

Apr 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...245l..19s&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 245, Apr. 1, 1981, p. L19-L22.

Astronomy and Astrophysics

Astronomy

58

Carbon Monoxide, Infrared Astronomy, Millimeter Waves, Molecular Clouds, Orion Nebula, Stellar Evolution, B Stars, High Resolution, Interstellar Matter, Microwave Emission, O Stars, Protostars, Shock Heating

Scientific paper

The results of high-spatial-resolution observations of the high-velocity 2.6-mm CO emission in the core of the Orion molecular cloud are presented. The location and size of the high-velocity CO region are compared with those of shock-heated H2 emission in order to decide whether the material is infalling to a centrally condensed object such as BN or IRc2 or outflowing from it. The CO high-velocity emission is found to be centered at the position of the BN object with error bars including IRc2 and inside the region of shock-heated H2 emission. The results imply that the primary dynamical process in the cloud core is an energetic outflow from one of the compact infrared sources. The short lifetime deduced for the high-velocity flow and the detection of similar phenomena in other nearby molecular clouds indicate that energetic outflows are common in molecular clouds and represent a stage in the pre-main-sequence of O and B stars. A mechanism for the driving force of an outflow due to infrared radiation pressure on grains in an envelope, at a radius of 3 x 10 to the 14th cm, optically thick to infrared radiation is also discussed.

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