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Exploring the early Universe with extremely metal-poor stars

Published online by Cambridge University Press:  09 May 2016

Terese T. Hansen ,
Norbert Christlieb ,
Camilla J. Hansen  and
Timothy C. Beers
Terese T. Hansen
Affiliation:
Landessternwarte, Heidelberg University Königstuhl 12, 69117 Heidelberg, Germany email: thansen@lsw.uni-heidelberg.de
Norbert Christlieb
Affiliation:
Landessternwarte, Heidelberg University Königstuhl 12, 69117 Heidelberg, Germany email: thansen@lsw.uni-heidelberg.de
Camilla J. Hansen
Affiliation:
Dark Cosmology Center, Copenhangen University Juliane Maries vej 30, 2100 Copenhagen, Denmark. email: cjhansen@dark-cosmology.dk
Timothy C. Beers
Affiliation:
Department of Physics and JINA Center for the Evolution of the Elements, University of Notre Dame Notre Dame, IN 46556, USA email: tbeers@nd.edu
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Abstract

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The earliest phases of Galactical chemical evolution and nucleosynthesis can be investigated by studying the old metal-poor stars. It has been recognized that a large fraction of metal-poor stars possess significant over-abundances of carbon relative to iron. Here we present the results of a 23-star homogeneously analyzed sample of metal-poor candidates from the Hamburg/ESO survey. We have derived abundances for a large number of elements ranging from Li to Pb. The sample includes four ultra metal-poor stars ([Fe/H] < −4.0), six CEMP-no stars, five CEMP-s stars, two CEMP-r stars and two CEMP-r/s stars. This broad variety of the sample stars gives us an unique opportunity to explore different abundance patterns at low metallicity.

Keywords

Galaxy: formation – Galaxy: halo – Stars: abundances – Stars: chemically peculiar Binaries: spectroscopic – ISM: structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Issue S317: The General Assembly of Galaxy Halos: Structure, Origin and Evolution , August 2015 , pp. 64 - 68
Copyright
Copyright © International Astronomical Union 2016 

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