EPJ Web Conf.
Volume 260, 2022The 16th International Symposium on Nuclei in the Cosmos (NIC-XVI)
|Number of page(s)||4|
|Section||Underground Nuclear Astrophysics|
|Published online||24 February 2022|
Direct measurement of the 19F(p, αγ)16O reaction in JUNA
1 Key Laboratory of Beam Technology and Material Modification of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China
2 The Joint Institute for Nuclear Astrophysics, Department of Physics, University of Notre Dame, Notre Dame, Indiana 46556 USA
3 Extreme Light Infrastructure – Nuclear Physics, Horia Hulubei National Institute for R&D in Physics and Nuclear Engineering (IFIN-HH), Bucharest-Măgurele 077125, Romania
4 Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China
5 China Institute of Atomic Energy, Beijing 102413, China
6 College of Physics and Optoelectronic Engineering, Shenzhen University, Shenzhen 518060, China
7 Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, China
8 Yalong River Hydropower Development Company, Chengdu 610051, China
9 Beijing Radiation Center, Beijing 100875, China
* e-mail: firstname.lastname@example.org
Published online: 24 February 2022
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.
© The Authors, published by EDP Sciences, 2022
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