An asymptotic giant branch star as the source of the abundance pattern of hyper-metal-poor star HE 1327-2326
[Context] Understanding the most metal-poor objects is key to interpreting the nature of the first stars. HE 1327-2326 (HE 1327), with metallicity [Fe/H] = −5.2, is one of the most metal-poor stars detected and a candidate to be the offspring of the first stars. Numerous efforts have been made to re...
| Autores: | , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2025 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/411078 |
| Acceso en línea: | http://hdl.handle.net/10261/411078 https://api.elsevier.com/content/abstract/scopus_id/105022076915 |
| Access Level: | acceso abierto |
| Palabra clave: | Stars: abundances Stars: AGB and post-AGB Stars: individual: HE 1327-2326 Stars: peculiar |
| Sumario: | [Context] Understanding the most metal-poor objects is key to interpreting the nature of the first stars. HE 1327-2326 (HE 1327), with metallicity [Fe/H] = −5.2, is one of the most metal-poor stars detected and a candidate to be the offspring of the first stars. Numerous efforts have been made to reproduce its abundance pattern, especially with high-mass stars undergoing supernova (SN) explosions. However, no model satisfactorily explains its entire surface chemical composition. Aims. The characteristic high CNO pattern with [N/Fe] > [C/Fe] > [O/Fe], the light element ‘slide’ (between Na and Si), and the presence of Sr and Ba in HE 1327 is reminiscent of asymptotic giant branch (AGB) stars that undergo third dredge-up, hot-bottom burning, and s-processing – suggesting that these stars were the source of the chemistry of the star. We tested this hypothesis. |
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