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dc.contributor.authorBarstow, M.A.
dc.contributor.authorBannister, N.P.
dc.contributor.authorHolberg, J.B.
dc.contributor.authorHubeny, I.
dc.contributor.authorBruhweiler, F.C.
dc.contributor.authorNapiwotzki, R.
dc.date.accessioned2010-02-11T15:18:25Z
dc.date.available2010-02-11T15:18:25Z
dc.date.issued2001
dc.identifier.citationBarstow , M A , Bannister , N P , Holberg , J B , Hubeny , I , Bruhweiler , F C & Napiwotzki , R 2001 , ' Far-ultraviolet spectroscopy of the hot DA white dwarf WD 2218 706 (DeHt5) with STIS ' , Monthly Notices of the Royal Astronomical Society , vol. 325 , no. 3 , pp. 1149-1156 . https://doi.org/10.1046/j.1365-8711.2001.04533.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 175708
dc.identifier.otherPURE UUID: aad25bd4-3a83-4e1e-b2f7-789368465c4d
dc.identifier.otherdspace: 2299/4266
dc.identifier.otherScopus: 0041702344
dc.identifier.urihttp://hdl.handle.net/2299/4266
dc.description‘The definitive version is available at www.blackwell-synergy.com '. Copyright Blackwell Publishing. DOI: 10.1046/j.1365-8711.2001.04533.x [Full text of this article is not available in the UHRA]
dc.description.abstractWe report a study of the photospheric composition of the hot DA white dwarf WD 2218+706, which is also the central star of the old planetary nebula DeHt5. Helium is detected in the far-UV spectrum. In addition, the star clearly contains significant quantities of elements heavier than He at abundances generally a factor of 2 to 10 higher than those found in the archetypal heavy element-rich DA G191−B2B. This is the first detection of trace He using the He iiλ1640 line in an isolated DA white dwarf, but the low surface gravity is more indicative of a binary evolution route from the red giant branch rather than a path along the asymptotic giant branch (AGB) as a single star. However, the absence of any evidence for a companion star and the uncertainty in the measured mass for WD 2218+706 still allow the possibility of an origin along an AGB evolutionary track. We reanalyse the existing optical spectra of WD 2218+706 using our latest pure H and heavy element-rich model atmospheres, obtaining a good match between the observed and synthetic spectra with either set of models. We find little evidence of any inconsistency in the temperature required to fit individual Balmer lines, as reported elsewhere for this star. Any discrepancies we see are confined to the Hα line and the core of Hβ but they do not compromise our analysis.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.titleFar-ultraviolet spectroscopy of the hot DA white dwarf WD 2218 706 (DeHt5) with STISen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1046/j.1365-8711.2001.04533.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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