The HH 83 molecular cloud: Gone with the wind

Details The HH 83 molecular cloud: Gone with the wind The HH 83 molecular cloud: Gone with the wind

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...423..310b&link_type=abstract

The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 423, no. 1, p. 310-319

Other

12

Herbig-Haro Objects, Interstellar Matter, Molecular Clouds, Star Formation, Stellar Evolution, Stellar Winds, Emission Spectra, Kinematics, Stellar Mass

Scientific paper

The HH 83 optical outflow and its host cloud core has been mapped in the J = 1 approaches 0 and J = 2 approaches 1 transitions of CO and its isotopes. The (12)CO and (13)CO maps exhibit a hot spot, a column density enhancement, and increased velocity dispersion at the position of the young star driving the optical jet. The cloud exhibits an overall velocity gradient along its major axis, which if interpreted as rotation would be consistent with a rotation axis roughly aligned with the optical jet. The (13)CO line width and a region of enhanced velocity gradients surrounding HH 83 IR are used to constrain the mass of this star and surrounding gas. In addition to the compact core, several other sub-condensations in the HH 83 cloud have been identified in the (13)CO map. The cloud may contain a pair of cavities symmetrically located on either side of HH 83 IR that lie roughly along the axis defined by the optical jet. A very low velocity and poorly collimated molecular outflow with a large redshifted lobe and a small blueshifted one is associated with HH 83. This molecular outflow has one of the lowest terminal velocities of any known source (about 5 km/s), a small total mass (0.1 - 0.2 solar mass), and is one of the least energetic molecular flows (2 x 1043 ergs) known. In this system, the Herbig-Haro jet is the most energetic component and dominates the energy and momentum of the CO-emitting lobes. The outflow from HH 83 IR has 'blown out' of the HH 83 molecular cloud and may be interacting with predominantly atomic gas in the intercloud medium. The morphology and kinematics of the HH 83 outflow suggests that it may be in a late stage of evolution.

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