Measurement of the Ce 140 (n,y) cross section at n_TOF and its astrophysical implications for the chemical evolution of the universe
140 Ce (n, y) is a key reaction for slow neutron-capture (s-process) nucleosynthesis due to being a bottleneck in the reaction flow. For this reason, it was measured with high accuracy (uncertainty˜5%) at the n_TOF facility, with an unprecedented combination of a high purity sample and low neutron-s...
| Autores: | , , , , , , , , , , , , , , , |
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| Tipo de recurso: | artículo |
| Fecha de publicación: | 2024 |
| País: | España |
| Institución: | Universitat Politècnica de Catalunya (UPC) |
| Repositorio: | UPCommons. Portal del coneixement obert de la UPC |
| Idioma: | inglés |
| OAI Identifier: | oai:upcommons.upc.edu:2117/407738 |
| Acceso en línea: | https://hdl.handle.net/2117/407738 https://dx.doi.org/10.1103/PhysRevLett.132.122701 |
| Access Level: | acceso abierto |
| Palabra clave: | Nuclear astrophysics Nucleosynthesis Gamma rays Nuclear reactions Astrofísica nuclear Nucleosíntesi Raigs gamma Reaccions nuclears Àrees temàtiques de la UPC::Física::Astronomia i astrofísica |
| Sumario: | 140 Ce (n, y) is a key reaction for slow neutron-capture (s-process) nucleosynthesis due to being a bottleneck in the reaction flow. For this reason, it was measured with high accuracy (uncertainty˜5%) at the n_TOF facility, with an unprecedented combination of a high purity sample and low neutron-sensitivity detectors. The measured Maxwellian averaged cross section is up to 40% higher than previously accepted values. Stellar model calculations indicate a reduction around 20% of the s-process contribution to the Galactic cerium abundance and smaller sizeable differences for most of the heavier elements. No variations are found in the nucleosynthesis from massive stars. |
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