LUNA的17O(p,γ)18F反应中65 keV共振强度的首次直接测量

IF 1.7 4区物理与天体物理 Q2 PHYSICS, NUCLEAR

Nuclear Physics A Pub Date : 2025-04-14 DOI:10.1016/j.nuclphysa.2025.123099

D. Piatti, LUNA collaboration

{"title":"LUNA的17O(p,γ)18F反应中65 keV共振强度的首次直接测量","authors":"D. Piatti, LUNA collaboration","doi":"10.1016/j.nuclphysa.2025.123099","DOIUrl":null,"url":null,"abstract":"<div><div>A precise determination of the proton capture rates on oxygen is mandatory to predict the abundance ratios of oxygen isotopes in a stellar environment where the hydrogen burning is active. The 17O(p,γ)18F reaction, in particular, plays a crucial role in AGB nucleosynthesis as well as in explosive hydrogen burning occurring in novae and type I supernovae. At the temperature of interest for the former scenario (20 MK ≤ T ≤ 80 MK) the main contribution to the astrophysical reaction rate comes from the <math><msub><mrow><mi>E</mi></mrow><mrow><mi>r</mi></mrow></msub></math> = 64.5 keV resonance. The strength of this resonance is presently determined only through indirect measurements, with an adopted value ωγ = (1.6 ± 0.3) × 10−11 eV. A new high sensitivity setup has been installed at LUNA, located at Laboratori Nazionali del Gran Sasso. The underground location of LUNA 400kV guarantees a reduction of the cosmic ray background by several orders of magnitude. The residual background was further reduced by a dedicated shielding. On the other hand the 4π-BGO detector efficiency was optimized installing an aluminum target chamber and holder. With about 400 C accumulated on Ta2O5 targets, with nominal 17O enrichment of 90%, the LUNA collaboration has performed the first ever direct measurement of the 64.5 keV resonance strength.</div></div>","PeriodicalId":19246,"journal":{"name":"Nuclear Physics A","volume":"1060 ","pages":"Article 123099"},"PeriodicalIF":1.7000,"publicationDate":"2025-04-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"The challenging first direct measurement of the 65 keV resonance strength in the 17O(p,γ)18F reaction at LUNA\",\"authors\":\"D. Piatti, LUNA collaboration\",\"doi\":\"10.1016/j.nuclphysa.2025.123099\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<div><div>A precise determination of the proton capture rates on oxygen is mandatory to predict the abundance ratios of oxygen isotopes in a stellar environment where the hydrogen burning is active. The 17O(p,γ)18F reaction, in particular, plays a crucial role in AGB nucleosynthesis as well as in explosive hydrogen burning occurring in novae and type I supernovae. At the temperature of interest for the former scenario (20 MK ≤ T ≤ 80 MK) the main contribution to the astrophysical reaction rate comes from the <math><msub><mrow><mi>E</mi></mrow><mrow><mi>r</mi></mrow></msub></math> = 64.5 keV resonance. The strength of this resonance is presently determined only through indirect measurements, with an adopted value ωγ = (1.6 ± 0.3) × 10−11 eV. A new high sensitivity setup has been installed at LUNA, located at Laboratori Nazionali del Gran Sasso. The underground location of LUNA 400kV guarantees a reduction of the cosmic ray background by several orders of magnitude. The residual background was further reduced by a dedicated shielding. On the other hand the 4π-BGO detector efficiency was optimized installing an aluminum target chamber and holder. With about 400 C accumulated on Ta2O5 targets, with nominal 17O enrichment of 90%, the LUNA collaboration has performed the first ever direct measurement of the 64.5 keV resonance strength.</div></div>\",\"PeriodicalId\":19246,\"journal\":{\"name\":\"Nuclear Physics A\",\"volume\":\"1060 \",\"pages\":\"Article 123099\"},\"PeriodicalIF\":1.7000,\"publicationDate\":\"2025-04-14\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Nuclear Physics A\",\"FirstCategoryId\":\"101\",\"ListUrlMain\":\"https://www.sciencedirect.com/science/article/pii/S0375947425000855\",\"RegionNum\":4,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q2\",\"JCRName\":\"PHYSICS, NUCLEAR\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Nuclear Physics A","FirstCategoryId":"101","ListUrlMain":"https://www.sciencedirect.com/science/article/pii/S0375947425000855","RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q2","JCRName":"PHYSICS, NUCLEAR","Score":null,"Total":0}

引用次数: 0

摘要

在氢燃烧活跃的恒星环境中，要预测氧同位素的丰度比，必须精确测定氧的质子俘获率。特别是17O(p,γ)18F反应，在AGB核合成以及新星和I型超新星中发生的爆炸性氢燃烧中起着至关重要的作用。在前一种情况下（20 MK≤T≤80 MK），天体物理反应速率的主要贡献来自Er = 64.5 keV共振。这种共振的强度目前只能通过间接测量来确定，采用的值ωγ =（1.6±0.3）× 10−11 eV。位于Gran Sasso国家实验室的LUNA上安装了一个新的高灵敏度装置。月球400kV的地下位置保证了宇宙射线背景的几个数量级的减少。专门的屏蔽进一步减少了残余背景。另一方面，采用铝制靶室和支架优化了4π-BGO探测器的效率。在Ta2O5目标上积累了大约400℃，标称富集了90%的17O， LUNA合作首次直接测量了64.5 keV的共振强度。

本文章由计算机程序翻译，如有差异，请以英文原文为准。

查看原文本刊更多论文

The challenging first direct measurement of the 65 keV resonance strength in the 17O(p,γ)18F reaction at LUNA

A precise determination of the proton capture rates on oxygen is mandatory to predict the abundance ratios of oxygen isotopes in a stellar environment where the hydrogen burning is active. The ¹⁷O(p,γ)¹⁸F reaction, in particular, plays a crucial role in AGB nucleosynthesis as well as in explosive hydrogen burning occurring in novae and type I supernovae. At the temperature of interest for the former scenario (20 MK ≤ T ≤ 80 MK) the main contribution to the astrophysical reaction rate comes from the

E_{r}

= 64.5 keV resonance. The strength of this resonance is presently determined only through indirect measurements, with an adopted value ωγ = (1.6 ± 0.3) × 10⁻¹¹ eV. A new high sensitivity setup has been installed at LUNA, located at Laboratori Nazionali del Gran Sasso. The underground location of LUNA 400kV guarantees a reduction of the cosmic ray background by several orders of magnitude. The residual background was further reduced by a dedicated shielding. On the other hand the 4π-BGO detector efficiency was optimized installing an aluminum target chamber and holder. With about 400 C accumulated on Ta₂O₅ targets, with nominal ¹⁷O enrichment of 90%, the LUNA collaboration has performed the first ever direct measurement of the 64.5 keV resonance strength.

求助全文

通过发布文献求助，成功后即可免费获取论文全文。去求助

来源期刊

Nuclear Physics A 物理-物理：核物理

CiteScore

3.60

自引率

7.10%

发文量

113

审稿时长

61 days

期刊介绍： Nuclear Physics A focuses on the domain of nuclear and hadronic physics and includes the following subsections: Nuclear Structure and Dynamics; Intermediate and High Energy Heavy Ion Physics; Hadronic Physics; Electromagnetic and Weak Interactions; Nuclear Astrophysics. The emphasis is on original research papers. A number of carefully selected and reviewed conference proceedings are published as an integral part of the journal.