dc.contributor.author | Oudmaijer, R.D. | |
dc.contributor.author | Proga, D. | |
dc.contributor.author | Drew, J.E. | |
dc.contributor.author | de Winter, D. | |
dc.date.accessioned | 2008-01-03T16:35:23Z | |
dc.date.available | 2008-01-03T16:35:23Z | |
dc.date.issued | 1998 | |
dc.identifier.citation | Oudmaijer , 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.issn | 0035-8711 | |
dc.identifier.other | dspace: 2299/1321 | |
dc.identifier.other | ORCID: /0000-0003-1192-7082/work/62750159 | |
dc.identifier.uri | http://hdl.handle.net/2299/1321 | |
dc.description | The definitive version is available at www.blackwell-synergy.com. Copyright Blackwell Publishing DOI : 10.1046/j.1365-8711.1998.01875.x | |
dc.description.abstract | New 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.format.extent | 572190 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | |
dc.title | The evolved B[e] star HD 87643: observations and a radiation-driven disc wind model for B[e] stars | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.description.status | Peer reviewed | |
rioxxterms.versionofrecord | 10.1046/j.1365-8711.1998.01875.x | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |