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dc.contributor.authorBurleigh, M.R.
dc.contributor.authorSaffer, R.
dc.contributor.authorGilmore, G.F.
dc.contributor.authorNapiwotzki, R.
dc.date.accessioned2008-01-25T10:11:22Z
dc.date.available2008-01-25T10:11:22Z
dc.date.issued1999
dc.identifier.citationBurleigh , M R , Saffer , R , Gilmore , G F & Napiwotzki , R 1999 , ' Optical spectroscopy of the candidate luminous white dwarf in the young Large Magellanic Cloud cluster NGC 1818 ' , Monthly Notices of the Royal Astronomical Society , vol. 310 , no. 1 , pp. L1L4 . https://doi.org/10.1046/j.1365-8711.1999.03123.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 146323
dc.identifier.otherPURE UUID: 5fb35050-d481-4f42-a3f1-b4d25f6b2e75
dc.identifier.otherdspace: 2299/1388
dc.identifier.otherScopus: 0041410261
dc.identifier.urihttp://hdl.handle.net/2299/1388
dc.descriptionThe definitive version is available at www.blackwell-synergy.com. Copyright Blackwell Publishing DOI : 10.1046/j.1365-8711.1999.03123.x
dc.description.abstractAn optical spectrum of the Elson et al. (1998) candidate luminous white dwarf in the young LMC cluster NGC1818 shows conclusively that it is not a degenerate star. A model atmosphere fit gives Teff 31,500K and log g 4.4, typical of a garden-variety main sequence B star. However, if it is a true LMC member then the star is underluminous by almost three magnitudes. Its position in the cluster colour-magnitude diagram also rules out the possibility that this is an ordinary B star. The luminosity is, however, consistent with a ~0.5M⊙ post-AGB or post-EHB object, although if it has evolved via single star evolution from a high mass (7.6−9.0M⊙) progenitor then we might expect it to have a much higher mass, ~0.9M⊙. Alternatively, it has evolved in a close binary. In this case the object offers no implications for the maximum mass for white dwarf progenitors, or the initial-final mass relation. Finally, we suggest that it could in fact be an evolved member of the LMC disk, and merely projected by chance onto NGC1818. Spectroscopically, though, we cannot distinguish between these evolutionary states without higher resolution (echelle) data.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.titleOptical spectroscopy of the candidate luminous white dwarf in the young Large Magellanic Cloud cluster NGC 1818en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1046/j.1365-8711.1999.03123.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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