Abstract
Observations of the CO (J = 1--0, lambda = 2.6 mm) high-velocity emission with the FCRAO 14 m antenna show it to be centered north of KL near the BN object with a radius of 1.3 x 10/sup 17/ cm. The error bars for this position include BN and IRc2. The shock-heated H/sub 2/ infrared emission surrounds the high-velocity CO. The primary dynamical process in the cloud core on the scale of 10/sup 17/ cm is an energetic outflow from either the BN object or IRc2. 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 cloud cores and represent a stage in the pre--main-sequence evolution of O and B stars. These energetic outflows are likely to be effective in stabilizing the parent molecular cloud against collapse. We also discuss 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/sup 14/ cm, optically thick to infrared radiation.
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