arXiv 1701.030882017-01nucl-ex

$^{30}$ S（$α$，p）反应速率的$^{30}$ S + PDMATHAAB共振弹性散射的首次测量

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

D. Kahl, H. Yamaguchi, S. Kubono, A. A. Chen, A. Parikh, D. N. Binh, J. Chen, S. Cherubini, N. N. Duy, T. Hashimoto, S. Hayakawa, N. Iwasa, H. S. Jung, S. Kato,… 展开作者

D. Kahl, H. Yamaguchi, S. Kubono, A. A. Chen, A. Parikh, D. N. Binh, J. Chen, S. Cherubini, N. N. Duy, T. Hashimoto, S. Hayakawa, N. Iwasa, H. S. Jung, S. Kato, Y. K. Kwon, S. Nishimura, S. Ota, K. Setoodehnia, T. Teranishi, H. Tokieda, T. Yamada, C. C. Yun, L. Y. Zhang

备注：: 16 pages, 12 figures
发表信息：: Phys. Rev. C 97, 015802 (2018)
DOI：: 10.1103/PhysRevC.97.015802

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摘要：

背景资料：I型x射线爆发是银河系中最常见的热核爆炸，由吸积中子星表面的热核失控引起。$^{30}$ S（$α$，p）反应在爆发模型中起着关键作用，但没有足够的实验信息来计算该反应的可靠、精确速率。目的：我们的测量是为了寻找$^{34}$ Ar中的态并确定它们的量子特性。特别是，自然宇称状态与大$α$衰变部分宽度应占主导地位的恒星反应速率。方法：我们进行了第一次测量的$^{30}$ S + $α$共振弹性散射的质心能量为5.5兆电子伏使用放射性离子束。实验采用了厚气体主动靶系统和硅探测器阵列在逆运动学。结果：在质心坐标系下，得到了$^{30}$ S（$α$，$α$）在$150^{\circ}$附近的一个激发函数。实验数据进行了分析与$R$-矩阵计算，我们观察到三个新的共振模式之间的11.1和12.1 MeV，提取其属性的共振能量，宽度，自旋和宇称。结论：我们计算的共振热核反应速率反应速率的$^{30}$ S（$α$，p）的基础上所有可用的实验数据的$^{34}$ Ar和发现一个上限约一个数量级大于使用统计模型确定的速率。这两个率的天体物理影响进行了研究，通过一个区域后处理I型X射线爆发计算。我们发现，我们的新上限的$^{30}$ S（$α$，p）$^{33}$ Cl率显着影响预测的核能产生率在爆发。

英文摘要：

Background: Type I x-ray bursts are the most frequent 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 an $R$-Matrix calculation, 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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