Other
Scientific paper
Nov 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.253..175s&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 253, Nov. 1, 1991, p. 175-183.
Other
41
Interstellar Matter, Molecular Clouds, Shock Wave Propagation, Abundance, Astronomical Models, Emission Spectra, H Lines, Line Spectra, Molecular Flow, Shock Absorbers
Scientific paper
This study presents the molecular and atomic fine structure signatures of planar shocks, bow shocks, and shock absorbers propagating within dense clouds and compares them with the powerful OMC-1 bipolar outflow. For fast-moving bows, line ratios are influenced only by the density, abundances, and bow shape. The 4.7-micron CO vibration-rotation band and the wide OH profiles are interpreted as emission from the molecular-atomic transition zone which divides the leading dissociated (J-shock) region from the pure H2 (C-shock) region in the bow flanks. It is demonstrated that the H2O emission line spectrum will also distinguish bows from planar shocks. Only the shock absorbers (bow shocks with a high magnetic field) yield H2, O I, and Co lines as wide as those observed in OMC-1. They are also distinguished by a relatively low proportion of low-J CO emission and other cool-gas discriminants due to the large magnetosonic Mach angle in the bow tails.
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