Aoki, W.; Frebel, A.; Christlieb, N.; Norris, J. E.; Beers, T. C.; Minezaki, T.; Barklem, P. S.; Honda, S.; Takada-Hidai, M.; Asplund, M.; Ryan, S.G.; Tsangarides, S.; Eriksson, K.; Steinhauer, A.; Deliyannis, C. P.; Nomoto, K.; Fujimoto, M. Y.; Ando, H.; Yoshii, Y. and Kajino, T.
He 1327-2326, an unevolved star with [Fe/H]<-5.0. I. A comprehensive abundance analysis.
Astrophysical Journal, 639(2) pp. 897–917.
We present the elemental abundances of HE 1327-2326, the most iron-deficient star known, determined from a comprehensive analysis of spectra obtained with the Subaru Telescope High Dispersion Spectrograph. HE 1327-2326 is either in its main-sequence or subgiant phase of evolution. Its non-LTE-corrected iron abundance is [Fe/H] = -5.45, 0.2 dex lower than that of HE 0107-5240, the previously most iron-poor object known, and more than 1 dex lower than those of all other metal-poor stars. Both HE 1327-2326 and HE 0107-5240 exhibit extremely large overabundances of carbon ([C/Fe] similar to +4). The combination of extremely high carbon abundance with outstandingly low iron abundance in these objects clearly distinguishes them from other metal-poor stars. The large carbon excesses in these two stars are not the result of a selection effect. There also exist important differences between HE 1327-2326 and HE 0107-5240. While the former shows remarkable overabundances of the light elements (N, Na, Mg, and Al), the latter shows only relatively small excesses of N and Na. The neutron-capture element Sr is detected in HE 1327-2326, but not in HE 0107-5240; its Sr abundance is significantly higher than the upper limit for HE 0107-5240. The Li I gamma 6707 line, which is detected in most metal-poor dwarfs and warm subgiants having the same temperature as HE 1327-2326, is not found in this object. The upper limit of its Li abundance [log epsilon(Li) < 1.5] is clearly lower than the Spite plateau value. These data provide new constraints on models of nucleosynthesis processes in the first-generation objects that were responsible for metal enrichment at the earliest times. We discuss possible scenarios to explain the observed abundance patterns.
||Halo galaxy; Nuclear reactions; Nucleosynthesis; Star Abundances; HE 1327–2326; Population II stars;
||Science > Physical Sciences
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