Abstract
The hypothesis that outflows driven by pre-main-sequence stellar winds are driving shells that fragment and energize molecular clouds, sustaining them so that they do not undergo free-fall collapse, leads to predicted correlations between line width, hydrogen density, and clump scale. Both the correlation scaling and normalization are in good accord with the correlations observed over a wide range of cloud scales. Implications are drawn for the efficiency of star formation and for cloud lifetimes.
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