Other
Scientific paper
Nov 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...310..820l&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 310, Nov. 15, 1986, p. 820-831.
Other
54
Hydrogen Clouds, Jet Flow, Molecular Clouds, Shock Waves, Star Formation, Continuous Spectra, Line Spectra, Mass Transfer, Velocity Distribution
Scientific paper
Extensive mapping of the 2 μm υ = 1-0 S(1) line of molecular hydrogen in the star-forming regions NGC 2071 and NGC 1333 (HH 12) is presented. In NGC 2071, the H2 emission indicates the presence of a pair of oppositely directed supersonic jets emerging from the newly formed cluster of stars at the center of the molecular cloud. The strongest of five emission peaks in this source occurs at the outer boundary of the high-velocity flow region mapped in CO. A gap in the H2 emission located directly to the southwest of the infrared cluster, provides additional supporting evidence for the existence of a massive circumstellar disk around NGC 2071. In HH 12 the S(1) line emission is closely correlated with the optical Herbig-Haro nebulosity, and peaks in the north; proper-motion measurements indicate that the HH object clumps are moving northward. In both outflows, the molecular hydrogen emission delineates the location where the kinetic energy of the high-velocity outflow is being converted into thermal energy by a shock wave and is radiated away. Results from a search of the S(1) line in other galactic and extragalactic star formation regions are briefly reported.
Bally John
Lane Adair P.
No associations
LandOfFree
Shocked molecular hydrogen and jets in star-forming clouds. II does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Shocked molecular hydrogen and jets in star-forming clouds. II, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Shocked molecular hydrogen and jets in star-forming clouds. II will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1148950