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Wang LH, Su J, Shen YP, He JJ, Lugaro M, Szányi B, Karakas AI, Zhang LY, Li XY, Guo B, Lian G, Li ZH, Wang YB, Chen LH, Cui BQ, Tang XD, Gao BS, Wu Q, Sun LT, Wang S, Sheng YD, Chen YJ, Zhang H, Li ZM, Song LY, Jiang XZ, Nan W, Nan WK, Zhang L, Cao FQ, Jiao TY, Ru LH, Cheng JP, Wiescher M, Liu WP. Measurement of the ^{18}O(α, γ)^{22}Ne Reaction Rate at JUNA and Its Impact on Probing the Origin of SiC Grains. Phys Rev Lett 2023; 130:092701. [PMID: 36930937 DOI: 10.1103/physrevlett.130.092701] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/27/2022] [Revised: 09/22/2022] [Accepted: 01/13/2023] [Indexed: 06/18/2023]
Abstract
The ^{18}O(α,γ)^{22}Ne reaction is critical for AGB star nucleosynthesis due to its connection to the abundances of several key isotopes, such as ^{21}Ne and ^{22}Ne. However, the ambiguous resonance energy and spin-parity of the dominant 470 keV resonance leads to substantial uncertainty in the ^{18}O(α,γ)^{22}Ne reaction rate for the temperature of interest. We have measured the resonance energies and strengths of the low-energy resonances in ^{18}O(α,γ)^{22}Ne at the Jinping Underground Nuclear Astrophysics experimental facility (JUNA) with improved precision. The key 470 keV resonance energy has been measured to be E_{α}=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 ^{18}O(α,γ)^{22}Ne 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 ^{21}Ne abundance predictions, with an impact on probing the origin of meteoritic stardust SiC grains from AGB stars.
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Affiliation(s)
- L H Wang
- Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China
| | - J Su
- Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China
| | - Y P Shen
- China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China
| | - J J He
- Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China
| | - M Lugaro
- Konkoly Observatory, Research Centre for Astronomy and Earth Sciences (CSFK), Eötvös Loránd Research Network (ELKH), Konkoly Thege Miklós út 15-17, 1121 Budapest, Hungary
- CSFK, MTA Centre of Excellence, Budapest, Konkoly Thege Miklós út 15-17, H-1121, Hungary
- ELTE Eötvös Loránd University, Institute of Physics, Budapest 1117, Pázmány Péter sétány 1/A, Hungary
- School of Physics and Astronomy, Monash University, Victoria 3800, Australia
| | - B Szányi
- Konkoly Observatory, Research Centre for Astronomy and Earth Sciences (CSFK), Eötvös Loránd Research Network (ELKH), Konkoly Thege Miklós út 15-17, 1121 Budapest, Hungary
- CSFK, MTA Centre of Excellence, Budapest, Konkoly Thege Miklós út 15-17, H-1121, Hungary
- Graduate School of Physics, University of Szeged, Dom tér 9, Szeged, 6720 Hungary
| | - A I Karakas
- School of Physics and Astronomy, Monash University, Victoria 3800, Australia
- ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia
| | - L Y Zhang
- Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China
| | - X Y Li
- Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China
| | - B Guo
- China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China
| | - G Lian
- China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China
| | - Z H Li
- China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China
| | - Y B Wang
- China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China
| | - L H Chen
- China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China
| | - B Q Cui
- China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China
| | - X D Tang
- Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China
| | - B S Gao
- Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China
| | - Q Wu
- Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China
| | - L T Sun
- Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China
| | - S Wang
- Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, China
| | - Y D Sheng
- Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China
| | - Y J Chen
- Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China
| | - H Zhang
- Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China
| | - Z M Li
- Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China
| | - L Y Song
- Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China
| | - X Z Jiang
- Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China
| | - W Nan
- China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China
| | - W K Nan
- China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China
| | - L Zhang
- China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China
| | - F Q Cao
- China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China
| | - T Y Jiao
- Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China
| | - L H Ru
- Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China
| | - J P Cheng
- Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China
| | - M Wiescher
- Department of Physics and The Joint Institute for Nuclear Astrophysics, University of Notre Dame, Notre Dame, Indiana 46556-5670, USA
- Wolfson Fellow of Royal Society, School of Physics and Astronomy, University of Edinburgh, King's Buildings, Edinburgh EH9 3FD, United Kingdom
| | - W P Liu
- China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China
- College of Science, Southern University of Science and Technology, Shenzhen 518055, China
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Zhang L, He J, deBoer RJ, Wiescher M, Heger A, Kahl D, Su J, Odell D, Chen Y, Li X, Wang J, Zhang L, Cao F, Zhang H, Zhang Z, Jiang X, Wang L, Li Z, Song L, Zhao H, Sun L, Wu Q, Li J, Cui B, Chen L, Ma R, Li E, Lian G, Sheng Y, Li Z, Guo B, Zhou X, Zhang Y, Xu H, Cheng J, Liu W. Measurement of 19F(p, γ)20Ne reaction suggests CNO breakout in first stars. Nature 2022; 610:656-660. [DOI: 10.1038/s41586-022-05230-x] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/28/2022] [Accepted: 08/11/2022] [Indexed: 11/09/2022]
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Gao B, Jiao TY, Li YT, Chen H, Lin WP, An Z, Ru LH, Zhang ZC, Tang XD, Wang XY, Zhang NT, Fang X, Xie DH, Fan YH, Ma L, Zhang X, Bai F, Wang P, Fan YX, Liu G, Huang HX, Wu Q, Zhu YB, Chai JL, Li JQ, Sun LT, Wang S, Cai JW, Li YZ, Su J, Zhang H, Li ZH, Li YJ, Li ET, Chen C, Shen YP, Lian G, Guo B, Li XY, Zhang LY, He JJ, Sheng YD, Chen YJ, Wang LH, Zhang L, Cao FQ, Nan W, Nan WK, Li GX, Song N, Cui BQ, Chen LH, Ma RG, Zhang ZC, Yan SQ, Liao JH, Wang YB, Zeng S, Nan D, Fan QW, Qi NC, Sun WL, Guo XY, Zhang P, Chen YH, Zhou Y, Zhou JF, He JR, Shang CS, Li MC, Kubono S, Liu WP, deBoer RJ, Wiescher M, Pignatari M. Deep Underground Laboratory Measurement of ^{13}C(α,n)^{16}O in the Gamow Windows of the s and i Processes. Phys Rev Lett 2022; 129:132701. [PMID: 36206440 DOI: 10.1103/physrevlett.129.132701] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/13/2021] [Revised: 04/01/2022] [Accepted: 06/01/2022] [Indexed: 06/16/2023]
Abstract
The ^{13}C(α,n)^{16}O reaction is the main neutron source for the slow-neutron-capture process in asymptotic giant branch stars and for the intermediate process. Direct measurements at astrophysical energies in above-ground laboratories are hindered by the extremely small cross sections and vast cosmic-ray-induced background. We performed the first consistent direct measurement in the range of E_{c.m.}=0.24 to 1.9 MeV using the accelerators at the China Jinping Underground Laboratory and Sichuan University. Our measurement covers almost the entire intermediate process Gamow window in which the large uncertainty of the previous experiments has been reduced from 60% down to 15%, eliminates the large systematic uncertainty in the extrapolation arising from the inconsistency of existing datasets, and provides a more reliable reaction rate for the studies of the slow-neutron-capture and intermediate processes along with the first direct determination of the alpha strength for the near-threshold state.
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Affiliation(s)
| | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | - R J deBoer
- Center for Nuclear Study, University of Tokyo, Wako, Saitama 351-0198, Japan
| | - M Wiescher
- Center for Nuclear Study, University of Tokyo, Wako, Saitama 351-0198, Japan
- Wolfson Fellow of Royal Society, School of Physics and Astronomy, University of Edinburgh, King's Buildings, Edinburgh EH9 3FD, United Kingdom
| | - M Pignatari
- Konkoly Observatory, Research Centre for Astronomy and Earth Sciences (CSFK), Eötvös Loránd Research Network (ELKH), Konkoly Thege Miklós út 15-17, H-1121 Budapest, Hungary
- CSFK, MTA Centre of Excellence, Budapest, Konkoly Thege Miklós út 15-17, Budapest H-1121, Hungary
- E. A. Milne Centre for Astrophysics, Department of Physics and Mathematics, University of Hull, Hull, HU6 7RX, United Kingdom
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Zhang L, Su J, He J, Wiescher M, deBoer R, Kahl D, Chen Y, Li X, Wang J, Zhang L, Cao F, Zhang H, Zhang Z, Jiao T, Sheng Y, Wang L, Song L, Jiang X, Li Z, Li E, Wang S, Lian G, Li Z, Tang X, Zhao H, Sun L, Wu Q, Li J, Cui B, Chen L, Ma R, Guo B, Xu S, Li J, Qi N, Sun W, Guo X, Zhang P, Chen Y, Zhou Y, Zhou J, He J, Shang C, Li M, Zhou X, Zhang Y, Zhang F, Hu Z, Xu H, Cheng J, Liu W. Direct measurement of the 19F( p, αγ) 16O reaction in JUNA. EPJ Web Conf 2022. [DOI: 10.1051/epjconf/202226008004] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
The 19F(p, αγ)16O reaction is of crucial importance for Galactic 19F abundances and CNO cycle loss in first generation Population III stars. Due to its extremely small cross sections, the 19F(p, αγ)16O reaction has not been measured in the low energy part of the Gamow window(70-200 keV). As a day-one campaign, the experiment was performed under the extremely low cosmicray-induced background environment of the China JinPing Underground Laboratory(CJPL), one of the deepest underground laboratories in the world. The γ-ray yields were measured over Ec.m. =72.4–344 keV, covering the full Gamow window for the first time. The direct experimental data will help people to expound the fluorine over-abundances, energy generation, as well as heavy-element nuclosynthesis scenario in asymptotic giant branch (AGB) stars, with the astrophysical model on the firm ground.
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Sergi ML, D’agata G, Guardo GL, Rapisarda GG, Burjan V, Cherubini S, Gulino M, Indelicato I, La Cognata M, Lamia L, Lattuada D, Mrázek J, Oliva AA, Pizzone RG, Romano S, Spartá R, Trippella O, Tumino A. Trojan Horse Investigation for AGB Stellar Nucleosynthesis. Universe 2022; 8:128. [DOI: 10.3390/universe8020128] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/10/2022]
Abstract
Asymptotic Giant Branch (AGB) stars are among the most important astrophysical sites influencing the nucleosynthesis and the chemical abundances in the Universe. From a pure nuclear point of view, several processes take part during this peculiar stage of stellar evolution thus requiring detailed experimental cross section measurements. Here, we report on the most recent results achieved via the application of the Trojan Horse Method (THM) and Asymptotic Normalization Coefficient (ANC) indirect techniques, discussing the details of the experimental procedure and the deduced reaction rates. In addition, we report also on the on going studies of interest for AGB nucleosynthesis.
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