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dc.contributor.authorBurton, M.
dc.contributor.authorHough, J.
dc.contributor.authorAxon, D.J.
dc.contributor.authorHasegawa, T.
dc.contributor.authorTamura, M.
dc.contributor.authorMcCaughrean, M.J.
dc.contributor.authorMcLean, I.
dc.date.accessioned2009-04-17T13:58:09Z
dc.date.available2009-04-17T13:58:09Z
dc.date.issued1988
dc.identifier.citationBurton , M , Hough , J , Axon , D J , Hasegawa , T , Tamura , M , McCaughrean , M J & McLean , I 1988 , ' Spectropolarimetry of the molecular-hydrogen line emission from OMC-1 ' , Monthly Notices of the Royal Astronomical Society , vol. 235 , no. 1 , pp. 161-174 .
dc.identifier.issn0035-8711
dc.identifier.otherdspace: 2299/3200
dc.identifier.urihttp://hdl.handle.net/2299/3200
dc.descriptionCopyright Royal Astronomical Society. [Full text of this article is not available in the UHRA]
dc.description.abstractObservations 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.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.titleSpectropolarimetry of the molecular-hydrogen line emission from OMC-1en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research (CAR)
dc.description.statusPeer reviewed
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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