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Cold massive cores are compared with their low mass counterparts using a 3D radiative transfer code to model observational line profile data. A major difference between the two types of object is that cold massive cores are much more turbulent than low mass starless cores. We suggest that this highly supersonic turbulence is best understood as being due to a large population of clumps embedded in a more tenuous medium. Many of these clumps will eventually undergo gravitational collapse to form individual low mass stars in a cluster around the massive stars.
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