The origin of HE0107-5240 and the production of O and Na in extremely metal-poor stars

Takuma Suda; Masayuki Aikawa; Takanori Nishimura; Masayuki Y. Fujimoto; Icko Iben Jr

doi:10.1016/j.nuclphysa.2005.05.061

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The origin of HE0107-5240 and the production of O and Na in extremely metal-poor stars

Takuma Suda·Masayuki Aikawa·Takanori Nishimura·Masayuki Y. Fujimoto·Icko Iben Jr

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Abstract

We elaborate the binary scenario for the origin of HE0107-5240, the most metal-poor star yet observed ([Fe/H] = -5.3), using current knowledge of the evolution of extremely metal-poor stars. From the observed C/N value, we estimate the binary separation and period. Nucleosynthesis in a helium convective zone into which hydrogen has been injected allows us to discuss the origin of surface O and Na as well as the abundance distribution of s-process elements. We can explain the observed abundances of 12C, 13C, N, O, and Na and predict future observations to validate the Pop III nature of HE0107-5240.

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Takuma Suda, Masayuki Aikawa, Takanori Nishimura, Masayuki Y. Fujimoto, Icko Iben Jr. 2005-04-25. The origin of HE0107-5240 and the production of O and Na in extremely metal-poor stars. https://doi.org/10.1016/j.nuclphysa.2005.05.061

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