First measurement of <math xmlns="http://www.w3.org/1998/Math/MathML"><mrow><mmultiscripts><mi mathvariant="normal">S</mi><mprescripts></mprescripts><none></none><mn>30</mn></mmultiscripts><mo>+</mo><mi>α</mi></mrow></math> resonant elastic scattering for the <math xmlns="http://www.w3.org/1998/Math/MathML"><mrow><mmultiscripts><mi mathvariant="normal">S</mi><mprescripts></mprescripts><none></none><mn>30</mn></mmultiscripts><mo>(</mo><mi>α</mi><mo>,</mo><mi>p</mi><mo>)</mo></mrow></math> reaction rate

D. Kahl; H. Yamaguchi (山口英斉; S. Kubono (久保野茂; A. A. Chen; A. Parikh; D. N. Binh; J. Chen (陈俊; S. Cherubini; N. N. Duy; T. Hashimoto (橋本尚志; S. Hayakawa (早川勢也; N. Iwasa (岩佐直仁; H. S. Jung (정효순; S. Kato (加藤静吾; Y. K. Kwon (권영관; S. Nishimura (西村俊二; S. Ota (大田晋輔; K. Setoodehnia; T. Teranishi (寺西高; H. Tokieda (時枝紘史; T. Yamada (山田拓; C. C. Yun (윤종철; L. Y. Zhang (张立勇

doi:10.1103/PhysRevC.97.015802

First measurement of ${}^{30}S + α$ resonant elastic scattering for the ${}^{30}S (α, p)$ reaction rate

D. Kahl^1,2,*, H. Yamaguchi (山口英斉)¹, S. Kubono (久保野茂)^1,3,4, A. A. Chen⁵, A. Parikh⁶, D. N. Binh^1,†, J. Chen (陈俊)^5,‡, S. Cherubini^7,8, N. N. Duy^9,10,§ et al.

T. Hashimoto (橋本尚志)^1,∥, S. Hayakawa (早川勢也)¹, N. Iwasa (岩佐直仁)¹¹, H. S. Jung (정효순)¹², S. Kato (加藤静吾)¹³, Y. K. Kwon (권영관)^12,∥, S. Nishimura (西村俊二)³, S. Ota (大田晋輔)¹, K. Setoodehnia^5,¶, T. Teranishi (寺西高)¹⁴, H. Tokieda (時枝紘史)¹, T. Yamada (山田拓)^11,#, C. C. Yun (윤종철)^12,∥, and L. Y. Zhang (张立勇)^4,**

¹Center for Nuclear Study (CNS), the University of Tokyo, RIKEN campus, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
²School of Physics & Astronomy, the University of Edinburgh, James Clerk Maxwell Building, Peter Guthrie Tait Road, Edinburgh EH9 3FD, United Kingdom
³RIKEN Nishina Center, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
⁴Institute of Modern Physics, Chinese Academy of Science, Nanchang Road 509, Lanzhou 730000, People's Republic of China
⁵Department of Physics & Astronomy, McMaster University, 1280 Main St West, Hamilton, Ontario L8S 4M1, Canada
⁶Departament de Física, Universitat Politècnica de Catalunya, c/Comte d'Urgell 187, Barcelona 08036, Spain
⁷Laboratori Nazionali del Sud-INFN, Catania 95123, Italy
⁸Dipartimento di Fisica e Astronomia, Università di Catania, Catania 95123, Italy
⁹Department of Physics, Dong Nai University, 4 Le Quy Don, Tan Hiep Ward, Bien Hoa City, Dong Nai, Vietnam
¹⁰Institute of Physics, Vietnam Academy of Science and Technology, 10 Dao Tan, Ba Dihn, Hanoi, Vietnam
¹¹Department of Physics, Tohoku University, Aoba, Sendai, Miyagi 980-8578, Japan
¹²Department of Physics, Chung-Ang University, Seoul 156-756, Republic of Korea
¹³Department of Physics, Yamagata University, 1-4-12 Kojirakawa-machi, Yamagata 990-8560, Japan
¹⁴Department of Physics, Kyushu University, 744 Motooka, Nishi-ku, Fukuoka 819-0395, Japan

^*daid.kahl@ed.ac.uk
^†Present address: 30 MeV Cyclotron Center, Tran Hung Dao Hospital, Hoan Kiem District, Hanoi, Vietnam.
^‡Present address: Nuclear Data Center, National Superconducting Cyclotron Laboratory, Michigan State University, 640 S. Shaw Ln, East Lansing, Michigan 48824, USA.
^§Present address: Department of Physics, Sungkyunkwan University, 300 Chunchun-dong, Jangan-ku, Suwon 400-746, Republic of Korea.
^∥Present address: Institute for Basic Science, Daejeon 305-811, Korea.
^¶Present address: Department of Physics, North Carolina State University, 2401 Stinson Dr, Raleigh, NC 27607, USA.
^#Present address: Yokohama Semiconductor Co., Ltd, Japan.
^**Present address: Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China.

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Phys. Rev. C 97, 015802 – Published 3 January, 2018

DOI: https://doi.org/10.1103/PhysRevC.97.015802

Abstract

Background: Type I x-ray bursts are the most frequently observed thermonuclear explosions in the galaxy, resulting from thermonuclear runaway on the surface of an accreting neutron star. The ${}^{30}S (α, p)$ reaction plays a critical role in burst models, yet insufficient experimental information is available to calculate a reliable, precise rate for this reaction.

Purpose: Our measurement was conducted to search for states in ${}^{34}{Ar}$ and determine their quantum properties. In particular, natural-parity states with large $α$ -decay partial widths should dominate the stellar reaction rate.

Method: We performed the first measurement of ${}^{30}S + α$ resonant elastic scattering up to a center-of-mass energy of 5.5 MeV using a radioactive ion beam. The experiment utilized a thick gaseous active target system and silicon detector array in inverse kinematics.

Results: We obtained an excitation function for ${}^{30}S (α, α)$ near $150^{\circ}$ in the center-of-mass frame. The experimental data were analyzed with $R$ -matrix calculations, and we observed three new resonant patterns between 11.1 and 12.1 MeV, extracting their properties of resonance energy, widths, spin, and parity.

Conclusions: We calculated the resonant thermonuclear reaction rate of ${}^{30}S (α, p)$ based on all available experimental data of ${}^{34}{Ar}$ and found an upper limit about one order of magnitude larger than a rate determined using a statistical model. The astrophysical impact of these two rates has been investigated through one-zone postprocessing type I x-ray burst calculations. We find that our new upper limit for the ${}^{30}S (α, p) {}^{33}{Cl}$ rate significantly affects the predicted nuclear energy generation rate during the burst.

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First measurement of ${}^{30}S + α$ resonant elastic scattering for the ${}^{30}S (α, p)$ reaction rate

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First measurement of S30+α resonant elastic scattering for the S30(α,p) reaction rate

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First measurement of ${}^{30}S + α$ resonant elastic scattering for the ${}^{30}S (α, p)$ reaction rate