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

  title={Astrophysics: How did the metals in a giant star originate?},
  author={Piercarlo Bonifacio and Marco Limongi and Alessandro Chieffi},
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… 
Limits on Population III star formation with the most iron-poor stars
We study the impact of star-forming minihaloes, and the initial mass function (IMF) of Population III (Pop III) stars, on the Galactic halo metallicity distribution function (MDF) and on the
ESPRESSO highlights the binary nature of the ultra-metal-poor giant HE 0107−5240
Context. The vast majority of the known stars of ultra low metallicity ([Fe/H] <  −4.5) are known to be enhanced in carbon, and belong to the “low-carbon band” (A(C) = log(C/H)+12 ≤ 7.6). It is
Probing the existence of very massive first stars
We present a novel approach aimed at identifying the key chemical elements to search for the (missing) descendants of very massive first stars exploding as Pair Instability Supernovae (PISN). Our
A CEMP-no star in the ultra-faint dwarf galaxy Pisces II
Aims. A probable carbon enhanced metal-poor (CEMP) star, Pisces II 10694, was discovered recently in the ultra-faint (UFD) galaxy Pisces II. This galaxy is supposed to be very old, suspected to
Primordial to extremely metal-poor AGB and Super-AGB stars: White dwarf or supernova progenitors?
Abstract Getting a better understanding of the evolution and nucleosynthetic yields of the most metal-poor stars (Z ≲ 10−5) is critical because they are part of the big picture of the history of the
Supernova dust yields: the role of metallicity, rotation, and fallback
Supernovae (SNe) are considered to have a major role in dust enrichment of high redshift galaxies and, due to the short lifetimes of interstellar grains, in dust replenishment of local galaxies. Here
TOPoS - II. On the bimodality of carbon abundance in CEMP stars Implications on the early chemical evolution of galaxies
Context. In the course of the TOPoS (Turn Off Primordial Stars) survey, aimed at discovering the lowest metallicity stars, we have found several carbon-enhanced metal-poor (CEMP) stars. These stars
An upper limit on the sulphur abundance in HE 1327-2326
Context: Star HE 1327-2326 is a unique object, with the lowest measured iron abundance ([Fe/H] ~ -6) and a peculiar chemical composition that includes large overabundances of C, N, and O with respect
Oxygen and light-element synthesis by neutron-capture reactions in metal-free and extremely metal-poor AGB stars
The metal-free (Population III: Pop. III) and extremely metal-poor (EMP) stars of low-and intermediate-masses experience mixing of hydrogen into the helium convection during the early TP-AGB phase,
Cosmic stellar relics in the Galactic halo
We study the stellar population history and chemical evolution of the Milky Way (MW) in a hierarchical Λ cold dark matter model for structure formation. Using a Monte Carlo method based on the


A stellar relic from the early Milky Way
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
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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