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Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006phdt.........4w&link_type=abstract
PhD Thesis, Proquest Dissertations And Theses 2006. Section 0051, Part 0606 167 pages; [Ph.D. dissertation].United States -- Co
Other
Protostellar Outflows, Star Formation, Molecular Clouds
Scientific paper
Star formation is a dynamic process in which newly formed stars interact with their parent molecular cloud. This feedback generates turbulence and gas motions which affects subsequent star formation within that cloud. Millimeter- wave observations of molecular clouds have revealed supersonic line widths, which are presumed to be due to turbulent motions. Supersonic turbulent energy, however, is expected to decay rapidly due to dissipation of energy in shocks.
If molecular clouds are long lived, then the turbulent motions must be constantly driven. On the other hand, if molecular clouds are destroyed on the scale of a few times the decay time, then the turbulence need not be driven, but the destruction mechanism must input significant energy and momentum into the cloud on that timescale. In either case, significant feedback must occur over a few Myr timescale. Protostellar outflows, collimated jets of material launched by accreting protostars, may be a significant source of feedback in regions which do not form high mass stars.
We explore different methods for probing the momentum injection rate of outflows and examine whether outflows can drive turbulence within the molecular cloud. On the scale of an entire molecular cloud, the shocks produced by outflows from young stars may not inject momentum at a sufficient rate to counter the rate at which momentum decays. However, intense outflow activity within individual cloud cores with high star formation rates, such as NGC 1333, may be sufficient to locally support or even disrupt the core.
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