Neutron-Capture Nucleosynthesis in Extremely Metal-Poor Stars - Application to the most iron-deficient stars HE0107-5240 and HE1327-2326

Details Neutron-Capture Nucleosynthesis in Extremely Metal-Poor Stars - Application to the most iron-deficient stars HE0107-5240 and HE1327-2326 Neutron-Capture Nucleosynthesis in Extremely Metal-Poor Stars - Application to the most iron-deficient stars HE0107-5240 and HE1327-2326

Feb 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aipc..891..397n&link_type=abstract

TOURS SYMPOSIUM ON NUCLEAR PHYSICS VI. AIP Conference Proceedings, Volume 891, pp. 397-400 (2007).

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Nucleosynthesis In Novae, Supernovae, And Other Explosive Environments, Radiative Capture, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, Population Iii Stars

Scientific paper

In extremely metal-poor stars ([Fe H]< 2 5), hydrogen is mixed into the convection driven by helium flash and induces neutron-capture nucleosynthesis with the reactions, 12C(p γ)13N(e+ν)13C(α n)16O, as the neutron source. We investigate the progress of this nucleosynthesis with use of nuclear network for a wide range of model parameters such as the amount of mixed hydrogen and the strength of helium flash. We reveal the characteristic abundance pattern from the light elements through the s-process elements, produced by alpha- and neutron-capture reactions under the extremely metal-poor condition. On the basis, we explore the possible modifications of surface abundances in the metal-free, Population III stars and discuss their relevance to the two most iron-deficient stars, HE0107-5240 and HE1327-2326, known to date.

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