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dc.contributor.authorOudmaijer, R.D.
dc.contributor.authorProga, D.
dc.contributor.authorDrew, J.E.
dc.contributor.authorde Winter, D.
dc.date.accessioned2008-01-03T16:35:23Z
dc.date.available2008-01-03T16:35:23Z
dc.date.issued1998
dc.identifier.citationOudmaijer , R D , Proga , D , Drew , J E & de Winter , D 1998 , ' The evolved B[e] star HD 87643: observations and a radiation-driven disc wind model for B[e] stars ' , Monthly Notices of the Royal Astronomical Society , vol. 300 , no. 1 , pp. 170-182 . https://doi.org/10.1046/j.1365-8711.1998.01875.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 141048
dc.identifier.otherPURE UUID: 703f70b9-ed16-4eb5-8d78-5be1b80107a4
dc.identifier.otherdspace: 2299/1321
dc.identifier.otherScopus: 0000235637
dc.identifier.urihttp://hdl.handle.net/2299/1321
dc.descriptionThe definitive version is available at www.blackwell-synergy.com. Copyright Blackwell Publishing DOI : 10.1046/j.1365-8711.1998.01875.x
dc.description.abstractNew high resolution spectroscopic and medium resolution spectropolarimetric data, complemented with optical broad and narrow band imaging, of the B[e] star HD 87643 are presented. The spectrum of HD 87643 exhibits the hybrid characteris- tics well known to be representative of the group of B[e] stars; a fast wind with an expansion velocity in excess of 1000 km s−1 is measured in the hydrogen and helium lines, while a slower component is traced by lower excitation lines and forbidden lines. Clues to the geometry of the rapidly expanding circumstellar shell are provided by the startling polarization changes across H . Comparison with published schematic calculations indicates that the polarizing material is located in a slowly rotating, ex- panding disk structure. A hydrodynamical model is then presented whose results are consistent with the original two-wind concept for B[e] stars and exhibits kinematic properties that may well explain the observed spectral features in HD 87643. The model calculations use as input a B star undergoing mass loss, surrounded by an op- tically thick disk. The resulting configuration consists of a fast polar wind from the star and a slowly expanding disk wind. The model also predicts that the stellar wind at intermediate latitudes is slower and denser than in the polar region.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.titleThe evolved B[e] star HD 87643: observations and a radiation-driven disc wind model for B[e] starsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1046/j.1365-8711.1998.01875.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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