The Nucleosynthetic Signatures of the First Star Survivors Among Hyper Metal-Poor Stars with [Fe/H]<-4.5

Details The Nucleosynthetic Signatures of the First Star Survivors Among Hyper Metal-Poor Stars with [Fe/H]<-4.5 The Nucleosynthetic Signatures of the First Star Survivors Among Hyper Metal-Poor Stars with [Fe/H]<-4.5

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc.1016...43s&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: The 10th International Symposium on Origin of Matter and Evolution of Galaxies: From

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Cosmology, Stellar Clusters And Associations, Galactic Halo

Scientific paper

The first stars in our Universe (Population III) are the useful probes for the star formation history in the very early Universe. These stars were born in the primordial gas cloud produced soon after the Big Bang and considered to be metal-free, i.e., comletely lack of elements heavier than lithium. In order to identify these survivors, we should consider the effect of changing surface abundances during their long lives. The surface abundances are modified by the accretion of gas from the interstellar matter and/or the binary mass transfer. The former possibly affects the iron group elements through the pollution of the parent cloud with the ejecta of supernovae. On the other hand, the latter can affect the abundance pattern of light and s-process elements through the evolution of primary star that experienced the internal mixing and dredge-up during thermally pulsating AGB before the final mass loss. The top three of the iron deficient stars HE1327-2326, HE0107-5240, and HE0557-4840 are reported as the candidates of the first stars by the current observations of extremely metal-poor stars in the Galactic halo. These stars have [Fe/H]<-4.5 and share the common feature of large enhancement of C. We argue that these abundance patterns are testified to the evolutionary characteristics of the first stars with low- and intermediate-mass by trying to constrain the mass of primary under the assumuption that they were the suvivors of secondary stars in the binary system when they were born. We also argue that the binary scenario for these stars are validated with the merging history of the Galaxy. The considerations of stellar evolution, nucleosynthesis, and Galactic chemical evolution reveal that these three stars are promising candidate for the first stars.

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