The molecular gas associated with HH46 and HH47

Details The molecular gas associated with HH46 and HH47 The molecular gas associated with HH46 and HH47

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987pasp...99..107k&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 99, Feb. 1987, p. 107-111.

Astronomy and Astrophysics

Astronomy

20

Interstellar Gas, Molecular Clouds, Pre-Main Sequence Stars, Stellar Envelopes, Abundance, Accretion Disks, Ammonia, Infrared Sources (Astronomy)

Scientific paper

The NASA 64-m and CSIRO 64-m antennas at Tidbinbilla and Parkes, respectively, have been used to observe the star-forming region associated with HH 46 and HH 47 in the Bok globule known as ESO 210-6A or Sa III. The (1,1), (2,2), and (3,3) transitions of ammonia were observed at the position of the infrared point source which is the star energizing this complex. Ammonia was not detected at other nearby locations in the globule. The ammonia emission is attributed to a circumstellar toroid or disk with a gas temperature of 17±2K, a density of 7±2×104cm-3, a size of 6000 - 7500 AU, and a mass of 0.09 - 0.14 M_sun;, assuming an ammonia abundance of 10-7. Such a low disk mass may imply more than mere confinement as the mechanism for achieving high collimation observed in the outflow from this region.

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