Measurement of the 18O(α, γ )22Ne Reaction Rate at JUNA and Its Impact on Probing the Origin of SiC Grains

被引：15

作者：

Wang, L. H. ^{[1
]}

Su, J. ^{[1
]}

Shen, Y. P. ^{[2
]}

He, J. J. ^{[1
]}

Lugaro, M. ^{[3
,4
,5
,6
]}

Szanyi, B. ^{[7
]}

Karakas, A. I. ^{[8
]}

Zhang, L. Y. ^{[1
]}

Li, X. Y. ^{[1
]}

Guo, B. ^{[2
]}

Lian, G. ^{[2
]}

Li, Z. H. ^{[2
]}

Wang, Y. B. ^{[2
]}

Chen, L. H. ^{[2
]}

Cui, B. Q. ^{[2
]}

Tang, X. D. ^{[9
]}

Gao, B. S. ^{[9
]}

Wu, Q. ^{[9
]}

Sun, L. T. ^{[9
]}

Wang, S. ^{[10
]}

Sheng, Y. D. ^{[1
]}

Chen, Y. J. ^{[1
]}

Zhang, H. ^{[1
]}

Li, Z. M.

Song, L. Y. ^{[1
]}

Jiang, X. Z. ^{[1
]}

Nan, W. ^{[2
]}

Nan, W. K. ^{[2
]}

Zhang, L. ^{[2
]}

Cao, F. Q. ^{[2
]}

Jiao, T. Y.

Ru, L. H.

Cheng, J. P. ^{[1
]}

Wiescher, M. ^{[11
,12
,13
]}

Liu, W. P. ^{[2
,13
,14
]}

机构：

[1] Beijing Normal Univ, Coll Nucl Sci & Technol, Key Lab Beam Technol, Minist Educ, Beijing 100875, Peoples R China

[2] China Inst Atom Energy, POB 275 10, Beijing 102413, Peoples R China

[3] Eotvos Lorand Res Network ELKH, Res Ctr Astron & Earth Sci CSFK, Konkoly Observ, Konkoly Thege Mikl Ut 15-17, H-1121 Budapest, Hungary

[4] MTA Ctr Excellence, CSFK, Konkoly Thege Mikl Ut 15-17, H-1121 Budapest, Hungary

[5] Eotvos Lorand Univ, Inst Phys, Pazmany Peter Setany 1-A, H-1117 Budapest, Hungary

[6] Monash Univ, Sch Phys & Astron, Melbourne, Vic 3800, Australia

[7] Univ Szeged, Grad Sch Phys, Dom Ter 9, H-6720 Szeged, Hungary

[8] ARC Ctr Excellence All Sky Astrophys 3 Dimens AST, Mt Stromlo, Australia

[9] Chinese Acad Sci, Inst Modern Phys, Lanzhou 730000, Peoples R China

[10] Shandong Univ, Inst Space Sci, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai 264209, Peoples R China

[11] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA

[12] Univ Notre Dame, Joint Inst Nucl Astrophys, Notre Dame, IN 46556 USA

[13] Univ Edinburgh, Sch Phys & Astron, Royal Soc, Kings Bldg, Edinburgh EH9 3FD, Scotland

[14] Southern Univ Sci & Technol, Coll Sci, Shenzhen 518055, Peoples R China

来源：

PHYSICAL REVIEW LETTERS | 2023年 / 130卷 / 09期

基金：

中国国家自然科学基金; 国家重点研发计划; 澳大利亚研究理事会;

关键词：

S-PROCESS NUCLEOSYNTHESIS; NUCLEAR; CAPTURE; YIELDS; STARS;

D O I：

10.1103/PhysRevLett.130.092701

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

The O-18(alpha, gamma )Ne-22 reaction is critical for AGB star nucleosynthesis due to its connection to the abundances of several key isotopes, such as Ne-21 and Ne-22. However, the ambiguous resonance energy and spin-parity of the dominant 470 keV resonance leads to substantial uncertainty in the O-18(alpha, gamma )Ne-22 reaction rate for the temperature of interest. We have measured the resonance energies and strengths of the low -energy resonances in O-18(alpha, gamma )(22)2Ne at the Jinping Underground Nuclear Astrophysics experimental facility (JUNA) with improved precision. The key 470 keV resonance energy has been measured to be E-alpha = 474.0 +/- 1.1 keV, with such high precision achieved for the first time. The spin-parity of this resonance state is determined to be 1-, removing discrepancies in the resonance strengths in earlier studies. The results significantly improve the precision of the O-18(alpha, gamma )Ne-22 reaction rates by up to about 10 times compared with the previous data at typical AGB temperatures of 0.1-0.3 GK. We demonstrate that such improvement leads to precise Ne-21 abundance predictions, with an impact on probing the origin of meteoritic stardust SiC grains from AGB stars.

引用

页数：6

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