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• W2150182013 abstract "To study the interaction of star-formation and turbulent molecular cloud structuring, we analyse numer- ical models and observations of self-gravitating clouds using the -variance as statistical measure for structural characteristics. In the models we resolve the transition from purely hydrodynamic turbulence to gravitational collapse associated with the formation and mass growth of protostellar cores. We compare models of driven and freely decaying turbulence with and without magnetic elds. Self-gravitating supersonic turbulence always pro- duces a density structure that contains most power on the smallest scales provided by collapsed cores as soon as local collapse sets in. This is in contrast to non-self-gravitating hydrodynamic turbulence where the -variance is dominated by large scale structures. To detect this eect in star-forming regions observations have to resolve the high density contrast of protostellar cores with respect to their ambient molecular cloud. Using the 3 mm contin- uum map of a star-forming cluster in Serpens we show that the dust emission traces the full density evolution. On the contrary, the density range accessible by molecular line observations is insucient for this analysis. Only dust emission and dust extinction observations are able to to determine the structural parameters of star-forming clouds following the density evolution during the gravitational collapse." @default.
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• W2150182013 date "2001-12-01" @default.
• W2150182013 modified "2023-09-26" @default.
• W2150182013 title "On the structure of self-gravitating molecular clouds" @default.
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• W2150182013 doi "https://doi.org/10.1051/0004-6361:20011324" @default.
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