Observations of a curving molecular outflow from V380Ori-NE: further support for prompt entrainment in protostellar outflows

Details Observations of a curving molecular outflow from V380Ori-NE: further support for prompt entrainment in protostellar outflows Observations of a curving molecular outflow from V380Ori-NE: further support for prompt entrainment in protostellar outflows

Nov 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000mnras.318..952d&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 318, Issue 3, pp. 952-960.

Astronomy and Astrophysics

Astronomy

19

Circumstellar Matter, Ism: Individual: V380Ori-Ne, Ism: Jets And Outflows, Ism: Kinematics And Dynamics, Infrared: Ism: Lines And Bands, Infrared: Stars

Scientific paper

CO J=3-2 and 4-3 observations of V380Ori-NE reveal a highly collimated bipolar molecular outflow associated with a jet traced here in H2 1-0 S(1) line emission. The source of the flow is also detected at 450 and 850μm with SCUBA. The combined CO and near-IR observations offer compelling support for the prompt entrainment model of jet-driven molecular outflows. Not only are the H2 shock fronts spatially coincident with peaks in the CO outflow lobes, but the slope of the mass-velocity distribution in the flow, measured here at intervals along both flow lobes, also clearly decreases just behind the advancing shock fronts (and towards the ends of the flow lobes), as one would expect if the high-to-low velocity mass fraction was enhanced by the entraining shocks. We also find that both lobes of the CO outflow clearly deviate, by some 20°, from the H2 jet direction near the source. Both lobes may be being deflected at the locations of the observed H2 shock fronts, where they impact dense, ambient material. Alternatively, the almost point-symmetric CO flow pattern could be caused by precession at the source. The submillimetre (submm) data reveal the source of the outflow, V380Ori-NE. The 450- and 850-μm maps show an elongated peak superimposed on to an extensive pedestal of weaker emission. The major axis of the source is oriented parallel with the inner flow axis. Indeed, weak 850-μm emission is detected along much of the bipolar outflow, particularly in the southern lobe and towards the southernmost CO intensity peak. The submm `continuum' data therefore probably trace warm dust and CO associated with the outflow. These data also confirm the status of V380Ori-NE as a Class I protostar. Overall, the orientation, simplicity and symmetry of this outflow, combined with the remarkable strength of the high-velocity line-wing emission in comparison to the ambient emission, make this system a perfect laboratory for future detailed studies of bipolar molecular outflows and their association with collimated jets from young, deeply embedded protostars.

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