Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.7607d&link_type=abstract
American Astronomical Society, AAS Meeting #211, #76.07; Bulletin of the American Astronomical Society, Vol. 39, p.867
Astronomy and Astrophysics
Astronomy
Scientific paper
Although most stars form in clusters, clustered star formation is still poorly understood. Protostellar winds, jets, and bipolar outflows are thought to be the primary drivers of turbulence in low-mass star forming clouds. These winds then act to redistribute energy and momentum throughout the cloud, in cases either decreasing or enhancing the local efficiency of star formation. The effects and observational signatures of these interactions in cluster forming regions are difficult to surmise observationally, however hydrodynamic models are evolving to the point where the interaction of winds and molecular cloud cores can be investigated and understood. This study presents an investigation of hydrodynamic models of wind-driven molecular cloud collapse by creating synthetic observations of those clouds using radiative transfer techniques. These synthetic observations are analyzed to find characteristics which distinguish them from isolated collapsing molecular cloud cores. There appear to be several characteristics of wind-driven gravitationally bound star forming cores that can be seen in the millimeter and submillimeter rotational transitions of relatively abundant molecular species within these clouds. These cores tend to have well ordered centroid velocity gradients, while those cores that are disrupted by winds tend to show chaotic centroid velocity gradients. The line profiles of the model gravitationally bound cores tend to be more symmetric and less self-absorbed than similar isolated gravitationally bound clouds. The wind-driven cores also tend to show very low-intensity high velocity molecular gas flowing off of the outer layers of the core with velocity increasing approximately linearly with angular distance from the core.
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