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

Autor: Wang LH; Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China., Su J; Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China., Shen YP; China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China., He JJ; Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China., Lugaro M; 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., Szányi B; 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., Karakas AI; School of Physics and Astronomy, Monash University, Victoria 3800, Australia.; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia., Zhang LY; Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China., Li XY; Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China., Guo B; China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China., Lian G; China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China., Li ZH; China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China., Wang YB; China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China., Chen LH; China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China., Cui BQ; China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China., Tang XD; Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China., Gao BS; Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China., Wu Q; Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China., Sun LT; Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China., Wang S; Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, China., Sheng YD; Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China., Chen YJ; Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China., Zhang H; Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China., Li ZM; Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China., Song LY; Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China., Jiang XZ; Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China., Nan W; China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China., Nan WK; China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China., Zhang L; China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China., Cao FQ; China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China., Jiao TY; Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China., Ru LH; Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China., Cheng JP; Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China., Wiescher M; 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., Liu WP; 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.
Jazyk: angličtina
Zdroj: Physical review letters [Phys Rev Lett] 2023 Mar 03; Vol. 130 (9), pp. 092701.
DOI: 10.1103/PhysRevLett.130.092701
Abstrakt: 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.
Databáze: MEDLINE