CO J = 2-1 observations of the NGC 2071 molecular outflow - A wind-driven shell

Details CO J = 2-1 observations of the NGC 2071 molecular outflow - A wind-driven shell CO J = 2-1 observations of the NGC 2071 molecular outflow - A wind-driven shell

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...347..358m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 347, Dec. 1, 1989, p. 358-364.

Other

54

Carbon Monoxide, Molecular Clouds, Nebulae, Reflection Nebulae, Stellar Winds, Astronomical Spectroscopy, Emission Spectra, Interstellar Masers, Stellar Envelopes, Stellar Luminosity, Water Masers

Scientific paper

Complete maps of the high-velocity (C-12)O J = 2-1 emission from the NGC 2071 bipolar molecular outflow are presented. The molecular outflow has a closed shell morphology similar to L1551 but is much more inclined out of the plane of the sky. Despite being driven by a source an order of magnitude more luminous than L1551, the molecular outflow is only moderately more massive, and its momentum and energy are very similar. The NGC 2071 outflow has a number of large-velocity-dispersion clumps, one of which may be where a stellar wind jet impacts the end wall of the lobe cavity. Two others, coincident with an H2O maser and dense high-velocity gas, may be fragments of circumstellar material which has become entrained in the stellar wind. It is believed that the morphology of molecular outflows is well understood by a model of an expanding molecular shell driven by a stellar wind, and that differences in the velocity structure, collimation, and lobe overlap of a wide variety of outflows may be largely due to the inclination angle in which the outflow is viewed.

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