Using 19F(3He,t)19Ne*(γ) to study astrophysically important levels near the 18F+p threshold

25TH INTERNATIONAL CONFERENCE ON THE APPLICATION OF ACCELERATORS IN RESEARCH AND INDUSTRY Pub Date : 2019-10-02 DOI:10.1063/1.5127732

M. Hall, D. Bardayan, S. Ahn, J. Allen, J. T. Anderson, A. D. Ayangeakaa, T. Baugher, J. Blackmon, D. Blankstein, S. Burcher, M. Carpenter, S. Cha, K. Chae, K. Chipps, J. Cizewski, M. Febbraro, B. Frentz, O. Hall, S. Henderson, J. Hu, C. Jiang, K. Jones, E. J. Lee, A. Lepailleur, D. S. Monteiro, P. O’Malley, S. Ota, S. Pain, B. Rasco, A. Ratkiewicz, J. Riggins, D. Santiago-Gonzalez, D. Seweryniak, A. Simon, H. Sims, Karl Smith, W. Tan, P. Thompson, C. Thornsberry, R. Torres-Isea, B. V. Kolk, R. Varner, D. Walter, G. Wilson, S. Zhu

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引用次数: 1

Abstract

A direct test of nova explosion models comes from the observation of γ rays created in the decay of radioactive isotopes produced in the nova. One such isotope, 18F, is believed to be the main source of observable γ rays at and below 511 keV. The main destruction mechanism of 18F is thought to be the 18F(p,α)15O reaction, and uncertainties in the reaction rate arise from uncertainties in the energies, spins, and parities of the nuclear levels in 19Ne above the 18F+p threshold. To measure the properties of these levels, the 19F(3He,t)19Ne∗(γ) reaction was studied at Argonne National Laboratory and the Nuclear Science Laboratory at the University of Notre Dame.A direct test of nova explosion models comes from the observation of γ rays created in the decay of radioactive isotopes produced in the nova. One such isotope, 18F, is believed to be the main source of observable γ rays at and below 511 keV. The main destruction mechanism of 18F is thought to be the 18F(p,α)15O reaction, and uncertainties in the reaction rate arise from uncertainties in the energies, spins, and parities of the nuclear levels in 19Ne above the 18F+p threshold. To measure the properties of these levels, the 19F(3He,t)19Ne∗(γ) reaction was studied at Argonne National Laboratory and the Nuclear Science Laboratory at the University of Notre Dame.

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使用19F(3He,t)19Ne*(γ)来研究18F+p阈值附近的天体物理重要水平

对新星爆炸模型的直接测试来自对新星产生的放射性同位素衰变中产生的γ射线的观察。其中一种同位素，18F，被认为是511kev及以下的可观测γ射线的主要来源。18F的主要破坏机制被认为是18F(p，α)15O反应，反应速率的不确定性来自于19Ne中超过18F+p阈值的核能级的能量、自旋和对偶的不确定性。为了测量这些能级的性质，在阿贡国家实验室和圣母大学的核科学实验室研究了19F(3He,t)19Ne * (γ)反应。对新星爆炸模型的直接测试来自对新星产生的放射性同位素衰变中产生的γ射线的观察。其中一种同位素，18F，被认为是511kev及以下的可观测γ射线的主要来源。18F的主要破坏机制被认为是18F(p，α)15O反应，反应速率的不确定性来自于19Ne中超过18F+p阈值的核能级的能量、自旋和对偶的不确定性。为了测量这些能级的性质，在阿贡国家实验室和圣母大学的核科学实验室研究了19F(3He,t)19Ne * (γ)反应。

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25TH INTERNATIONAL CONFERENCE ON THE APPLICATION OF ACCELERATORS IN RESEARCH AND INDUSTRY

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