The $^{22}$Ne($α$,n)$^{25}$Mg reaction -- state of the art, astrophysics, and perspectives
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arXiv
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| Main Authors: | , , , , , , , , , , , , , |
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| Format: | Preprint |
| Published: |
2025
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| _version_ | 1866916743612465152 |
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| author | Best, Andreas Adsley, Philip Amberger, Ryan Battino, Umberto Chillery, Thomas La Cognata, Marco deBoer, Richard James Mercogliano, Daniela Ota, Shuya Rapagnani, David Sidhu, Ragandeep Singh Spartà, Roberta Tumino, Aurora Wiescher, Michael |
| author_facet | Best, Andreas Adsley, Philip Amberger, Ryan Battino, Umberto Chillery, Thomas La Cognata, Marco deBoer, Richard James Mercogliano, Daniela Ota, Shuya Rapagnani, David Sidhu, Ragandeep Singh Spartà, Roberta Tumino, Aurora Wiescher, Michael |
| contents | One of the most important stellar neutron sources is the $^{22}$Ne($α$,n)$^{25}$Mg reaction, which gets activated both during the helium intershell burning in asymptotic giant branch stars and in core helium and shell carbon burning in massive stars. The $^{22}$Ne($α$,n)$^{25}$Mg reaction serves as the main neutron producer for the weak s-process and provides a short but strong neutron exposure during the helium flash phase of the main s-process, significantly affecting the abundances at the s-process branch points. The cross section needs to be known at very low energies, as close as possible to the neutron threshold at $E_α= 562$ keV ($Q = - 478$ keV), but both direct and indirect measurements have turned out to be very challenging, leading to significant uncertainties. Here we discuss the current status of the reaction, including recent and upcoming measurements, and provide a discussion on the astrophysical implications as well as an outlook into the near future. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2505_12008 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The $^{22}$Ne($α$,n)$^{25}$Mg reaction -- state of the art, astrophysics, and perspectives Best, Andreas Adsley, Philip Amberger, Ryan Battino, Umberto Chillery, Thomas La Cognata, Marco deBoer, Richard James Mercogliano, Daniela Ota, Shuya Rapagnani, David Sidhu, Ragandeep Singh Spartà, Roberta Tumino, Aurora Wiescher, Michael Nuclear Experiment One of the most important stellar neutron sources is the $^{22}$Ne($α$,n)$^{25}$Mg reaction, which gets activated both during the helium intershell burning in asymptotic giant branch stars and in core helium and shell carbon burning in massive stars. The $^{22}$Ne($α$,n)$^{25}$Mg reaction serves as the main neutron producer for the weak s-process and provides a short but strong neutron exposure during the helium flash phase of the main s-process, significantly affecting the abundances at the s-process branch points. The cross section needs to be known at very low energies, as close as possible to the neutron threshold at $E_α= 562$ keV ($Q = - 478$ keV), but both direct and indirect measurements have turned out to be very challenging, leading to significant uncertainties. Here we discuss the current status of the reaction, including recent and upcoming measurements, and provide a discussion on the astrophysical implications as well as an outlook into the near future. |
| title | The $^{22}$Ne($α$,n)$^{25}$Mg reaction -- state of the art, astrophysics, and perspectives |
| topic | Nuclear Experiment |
| url | https://arxiv.org/abs/2505.12008 |