| dc.contributor.author | Burton, M. | |
| dc.contributor.author | Hough, J. | |
| dc.contributor.author | Axon, D.J. | |
| dc.contributor.author | Hasegawa, T. | |
| dc.contributor.author | Tamura, M. | |
| dc.contributor.author | McCaughrean, M.J. | |
| dc.contributor.author | McLean, I. | |
| dc.date.accessioned | 2009-04-17T13:58:09Z | |
| dc.date.available | 2009-04-17T13:58:09Z | |
| dc.date.issued | 1988 | |
| dc.identifier.citation | Burton , 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.issn | 0035-8711 | |
| dc.identifier.other | dspace: 2299/3200 | |
| dc.identifier.uri | http://hdl.handle.net/2299/3200 | |
| dc.description | Copyright Royal Astronomical Society. [Full text of this article is not available in the UHRA] | |
| dc.description.abstract | Observations 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.iso | eng | |
| dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | |
| dc.title | Spectropolarimetry of the molecular-hydrogen line emission from OMC-1 | en |
| dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
| dc.contributor.institution | Centre for Astrophysics Research (CAR) | |
| dc.description.status | Peer reviewed | |
| rioxxterms.type | Journal Article/Review | |
| herts.preservation.rarelyaccessed | true | |
