AAS 199th meeting, Washington, DC, January 2002
Session 60. Star Formation - Accretion and Outflow
Display, Tuesday, January 8, 2002, 9:20am-6:30pm, Exhibit Hall

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[60.07] CO outflows from YSO

C.F. Lee, L.G. Mundy, J.M. Stone, E.C. Ostriker (University of Maryland, College Park)

We have mapped the CO J=1-0 emission from molecular outflows associated with six young stellar systems using the BIMA array. The systems, L 723, IRAM 04191, L 1641S, HH 114/115, L 1221 and RNO 91, are all relatively nearby, low luminosity and range from Class 0 to Class II sources. L 723 and L 1221 are found to be pairs of bipolar outflows. Generally, the CO outflow forms a shell structure around the outflow axis with the higher velocity emission further out from the source. For some outflows, e.g., L 723 and RNO 91, although there are no H2 bow shock structures detected along the outflow axis, there are clumpy and bow-like structures in CO along the outflow axis within the shell. Comparing the observed outflow features to that of the jet- and wind-driven models, we find that the outflow systems show some features that are characteristic of the jet-driven model and some features that are characteristic of the wind-driven model. However, neither model can fully explain the kinematic features of these outflows. In addition, the jet-driven model may need jet wandering to produce the observed outflow width and momentum for most of these outflows, while the wind-driven model may need a collimated core with strong velocity gradient away from the core to produce the highly collimated outflows and the observed curved internal H2 bow shock structures.

The author(s) of this abstract have provided an email address for comments about the abstract: chinfei@astro.umd.edu

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