| Article ID | Journal | Published Year | Pages | File Type |
|---|---|---|---|---|
| 9850971 | Nuclear Physics A | 2005 | 4 Pages |
Abstract
We elaborate the binary scenario for the origin of HE0107-5240, the most metal-poor star yet observed ([Fe/H] = â5.3), 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.
Related Topics
Physical Sciences and Engineering
Physics and Astronomy
Nuclear and High Energy Physics
Authors
T. Suda, M. Aikawa, T. Nishimura, M.Y. Fujimoto, I. Jr.,