| Issue |
EPJ Web Conf.
Volume 260, 2022
The 16th International Symposium on Nuclei in the Cosmos (NIC-XVI)
|
|
|---|---|---|
| Article Number | 11017 | |
| Number of page(s) | 6 | |
| Section | Poster | |
| DOI | https://doi.org/10.1051/epjconf/202226011017 | |
| Published online | 24 February 2022 | |
https://doi.org/10.1051/epjconf/202226011017
First direct limit on the 395 keV resonance of the 22Ne(α, γ)26Mg reaction
1 Università degli studi di Milano and INFN Sezione di Milano
2 https://luna.lngs.infn.it
* e-mail: eliana.masha@unimi.it
Published online: 24 February 2022
The 22Ne(α, γ)26Mg reaction (Q = 10614.74 keV) competes with the 22Ne(α, n)25Mg reaction (Q = −478.34 keV) which is the main source of neutrons for the s-process in low-mass Asymptotic Giant Branch and massive stars. The cross sections of these reactions are crucial to fix the cross over temperature at which (α, n) rate exceeds the (α, γ) one. Moreover, the uncertainty on the 22Ne(α, γ)26Mg reaction rate affects also the nucleosynthesis of isotopes between 26Mg and 31P in intermediate-mass stars.
At lower temperatures (T < 300 MK) where the (α, γ) channel is dominant, the rate of the 22Ne(α, γ)26Mg reaction is influenced by several resonances. The present study focuses on the Eα = 395 keV resonance which so far have been studied only indirectly leading to a wide range of possible values for its resonance strength (10−15 −10−9 eV).
The experiment has been completed at LUNA using the intense alpha beam of the LUNA 400 kV accelerator and a windowless differential-pumped gas target combined with a high efficiency BGO detector. Experimental details and preliminary results will be shown.
© The Authors, published by EDP Sciences, 2022
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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