A new sample of extremely/ultra metal-poor stars
Perez, A. E. Garcia; Christlieb, N.; Ryan, Sean 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.
Citation: Perez , 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 . , 10.1088/0031-8949/2008/T133/014036
A 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.
Original 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]
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