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dc.contributor.authorPerez, A. E. Garcia
dc.contributor.authorChristlieb, N.
dc.contributor.authorRyan, Sean G.
dc.contributor.authorBeers, T.C.
dc.contributor.authorAoki, W.
dc.contributor.authorAsplund, M.
dc.contributor.authorBarklem, P.S.
dc.contributor.authorBessell, M.S.
dc.contributor.authorEriksson, K.
dc.contributor.authorFrebel, A.
dc.contributor.authorGustafsson, B.
dc.contributor.authorKorn, A.J.
dc.contributor.authorNordstrom, B.
dc.contributor.authorNorris, J.E.
dc.date.accessioned2011-09-12T11:01:06Z
dc.date.available2011-09-12T11:01:06Z
dc.date.issued2008-12
dc.identifier.citationPerez , A E G , Christlieb , N , Ryan , S G , Beers , T C , Aoki , W , Asplund , M , Barklem , P S , Bessell , M S , Eriksson , K , Frebel , A , Gustafsson , B , Korn , A J , Nordstrom , B & Norris , J E 2008 , ' A new sample of extremely/ultra metal-poor stars ' , Physica Scripta , vol. T133 , 014036 . https://doi.org/10.1088/0031-8949/2008/T133/014036
dc.identifier.issn0031-8949
dc.identifier.otherPURE: 348405
dc.identifier.otherPURE UUID: 3bb75069-4146-47a4-8ea3-8813e66fed5e
dc.identifier.otherWOS: 000262583700038
dc.identifier.otherScopus: 70350654387
dc.identifier.urihttp://hdl.handle.net/2299/6392
dc.descriptionOriginal article can be found at: http://www.iop.org/ Copyright Royal Swedish Academy of Sciences [Full text of this article is not available in the UHRA]
dc.description.abstractA sample of 30 very metal-poor stars from the Hamburg-European Southern Observatory (ESO) objective-prism survey have been observed at high spectral resolution at the Very Large Telescope (VLT) using the Ultraviolet and Visual Echelle Spectrograph (UVES). Two of the observed stars are very interesting not only because of their very low iron content, approximately four orders of magnitude lower than the solar value, but also because we detected the neutral lithium resonance line at 670.8 nm. Hydrogen lines suggest that the two observed stars have effective temperatures around 6000-6250K and according to isochrones, they are either on the main-sequence or on the subgiant branch, in which case they would probably be the most metal-poor dwarfs or warm subgiants with lithium detections known. These detections would allow to determine more accurately the slope of the trend of the lithium abundance with [Fe/H] than was possible with samples of unevolved stars restricted to higher metallicities.en
dc.language.isoeng
dc.relation.ispartofPhysica Scripta
dc.titleA new sample of extremely/ultra metal-poor starsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted2008-12
rioxxterms.versionofrecordhttps://doi.org/10.1088/0031-8949/2008/T133/014036
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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