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

被引：9

作者：

Kahl, D. ^{[1
,2
]}

Yamaguchi, H. ^{[1
]}

Kubono, S. ^{[1
,3
,4
]}

Chen, A. A. ^{[5
]}

Parikh, A. ^{[6
]}

Binh, D. N. ^{[1
,15
]}

Chen, J. ^{[5
,16
]}

Cherubini, S. ^{[7
,8
]}

Duy, N. N. ^{[9
,10
,17
]}

Hashimoto, T. ^{[1
,18
]}

Hayakawa, S. ^{[1
]}

Iwasa, N. ^{[11
]}

Jung, H. S. ^{[12
]}

Kato, S. ^{[13
]}

Kwon, Y. K. ^{[12
,18
]}

Nishimura, S. ^{[3
]}

Ota, S. ^{[1
]}

Setoodehnia, K. ^{[5
,19
]}

Teranishi, T. ^{[14
]}

Tokieda, H. ^{[1
]}

Yamada, T. ^{[11
,20
]}

Yun, C. C. ^{[12
,18
]}

Zhang, L. Y. ^{[4
,21
]}

机构：

[1] Univ Tokyo, CNS, RIKEN campus,2-1 Hirosawa, Wako, Saitama 3510198, Japan

[2] Univ Edinburgh, Sch Phys & Astron, James Clerk Maxwell Bldg,Peter Guthrie Tait Rd, Edinburgh EH9 3FD, Midlothian, Scotland

[3] RIKEN Nishina Ctr, 2-1 Hirosawa, Wako, Saitama 3510198, Japan

[4] Chinese Acad Sci, Inst Modern Phys, Nanchang Rd 509, Lanzhou 730000, Gansu, Peoples R China

[5] McMaster Univ, Dept Phys & Astron, 1280 Main St West, Hamilton, ON L85 4M1, Canada

[6] Univ Politecn Cataluna, Dept Fis, C Comte Urgell 187, Barcelona 08036, Spain

[7] INFN, Lab Nazl Sud, I-95123 Catania, Italy

[8] Univ Catania, Dipartimento Fis & Astron, I-95123 Catania, Italy

[9] Dong Nai Univ, Dept Phys, 4 Le Quy Don, Bien Hoa City, Dong Nai, Vietnam

[10] Vietnam Acad Sci & Technol, Inst Phys, 10 Dao Tan, Hanoi, Vietnam

[11] Tohoku Univ, Dept Phys, Aoba Ku, Sendai, Miyagi 9808578, Japan

[12] Chung Ang Univ, Dept Phys, Seoul 56756, South Korea

[13] Yamagata Univ, Dept Phys, 1-4-12 Kojirakawa Machi, Yamagata 9908560, Japan

[14] Kyushu Univ, Dept Phys, Nishi Ku, 744 Motooka, Fukuoka 8190395, Japan

[15] Tran Hung Dao Hosp, MeV Cyclotron Ctr 30, Hanoi, Vietnam

[16] Michigan State Univ, Nucl Data Ctr, Natl Superconducting Cyclotron Lab, 640 S Shaw Ln, E Lansing, MI 48824 USA

[17] Sungkyunkwan Univ, Dept Phys, 300 Chunchun Dong, Suwon 400746, South Korea

[18] Inst for Basic Sci Korea, Daejeon 305811, South Korea

[19] North Carolina State Univ, Dept Phys, 2401 Stinson Dr, Raleigh, NC 27607 USA

[20] Yokohama Semicond Co Ltd, Yokohama, Kanagawa, Japan

[21] Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ, Beijing 100012, Peoples R China

来源：

PHYSICAL REVIEW C | 2018年 / 97卷 / 01期

基金：

英国科学技术设施理事会; 加拿大自然科学与工程研究理事会;

关键词：

X-RAY-BURSTS; ACCRETING NEUTRON-STARS; NE-18(ALPHA; P)NA-21; REACTION; ELASTIC-SCATTERING; CROSS-SECTIONS; SEPARATOR CRIB; REACTION-RATES; RP-PROCESS; ALPHA; ASTROPHYSICS;

D O I：

10.1103/PhysRevC.97.015802

中图分类号：

O57 [原子核物理学、高能物理学];

学科分类号：

070202 ;

摘要：

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 S-30(alpha, 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 Ar-34 and determine their quantum properties. In particular, natural-parity states with large alpha-decay partial widths should dominate the stellar reaction rate. Method: We performed the firstmeasurement of S-30 + alpha 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 S-30(alpha,alpha) near 150 degrees. 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 30S(alpha, p) based on all available experimental data of Ar-34 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 S-30(alpha, p)Cl-33 rate significantly affects the predicted nuclear energy generation rate during the burst.

引用

页数：16

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