Astrophysics: How did the metals in a giant star originate?

@article{Bonifacio2003AstrophysicsHD,
  title={Astrophysics: How did the metals in a giant star originate?},
  author={Piercarlo Bonifacio and Marco Limongi and Alessandro Chieffi},
  journal={Nature},
  year={2003},
  volume={422},
  pages={834-834}
}
The chemical composition of stars with extremely low metal contents (taking 'metals' to mean all elements other than hydrogen and helium) provides us with information on the masses of the stars that produced the first metals. Such a direct connection is not possible, however, if the surface of the star has been polluted by enriched material, either dredged from the star's interior or transferred from a companion star. Here we argue that, in the case of HE0107–5240 (ref. 1), the most iron-poor… 
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References

SHOWING 1-6 OF 6 REFERENCES
A stellar relic from the early Milky Way
TLDR
This work reports the discovery of a low-mass star with an iron abundance as low as 1/200,000 of the solar value, which suggests that population III stars could still exist and that the first generation of stars also contained long-livedLow-mass objects.
Chemical Composition of the Carbon-rich, Extremely Metal Poor Star CS 29498–043: A New Class of Extremely Metal Poor Stars with Excesses of Magnesium and Silicon*
We analyze a high-resolution, high signal-to-noise ratio spectrum of the carbon-rich, extremely metal poor star CS 29498-043, obtained with the Subaru Telescope High Dispersion Spectrograph. We find
First Stars II. Elemental abundances in the extremely metal-poor star CS 22949-037 ? A diagnostic of early massive supernovae
CS 22949-037 is one of the most metal-poor giants known ((Fe=H) 4:0), and it exhibits large overabundances of carbon and nitrogen (Norris et al.). Using VLT-UVES spectra of unprecedented quality,
New quests in stellar astrophysics: the link between stars and cosmology : proceedings of the international conference held in Puerto Vallarta, México, 26-30 March 2001
Part I: Stellar Atmospheres. A Few Things We Do Not Know About Stars and Model Atmospheres R.L. Kurucz. Cool Stellar Atmospheres P.H. Hauschildt, et al. A Critical Appraisal of ATLAS9 and NextGen5
The Evolutionary Properties of Zero Metal Stars in the Mass Range between 4 and 100 M
In this review we will discuss the main evolutionary properties of the zero metallicity stars in the mass interval which extends from the intermediate mass to the massive stars together with their
The Explosive Yields Produced by the First Generation of Core Collapse Supernovae and the Chemical Composition of Extremely Metal Poor Stars
We present a detailed comparison of an extended set of elemental abundances observed in some of the most metal poor stars presently known and the ejecta produced by a generation of primordial core