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Spectropolarimetry of the molecular hydrogen line emission from OMC-1Observations of the H2 v = 1-0 S(1) line at 35 km/s velocity resolution were obtained at several locations within OMC-1, including the molecular hydrogen reflection nebula. All line profiles are smooth and show no evidence for being composed of discrete components. The data are discussed with respect to a model for the H2 line formation in which the emission originates in discrete clumps moving at different velocities. It is suggested that the extended blue wing may come from fast-moving clumps embedded in a wind.
Document ID
19890029438
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Burton, Michael G.
(NASA Ames Research Center Moffett Field, CA; Royal Observatory, Edinburgh, United Kingdom)
Hough, J. H.
(Hatfield Polytechnic United Kingdom)
Axon, David J.
(Manchester, Victoria University Jodrell Bank, United Kingdom)
Hasegawa, T.
(Nobeyama Radio Observatory Nagano, Japan)
Tamura, M.
(Kyoto University Japan)
Date Acquired
August 14, 2013
Publication Date
November 1, 1988
Publication Information
Publication: Royal Astronomical Society, Monthly Notices
Volume: 235
ISSN: 0035-8711
Subject Category
Astrophysics
Accession Number
89A16809
Distribution Limits
Public
Copyright
Other

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