通过费米能区重离子碰撞产额分布来研究16O原子核的团簇结构

近几年来,原子核核内的$\alpha$团簇结构引起了人们的广泛关注。本工作的目的是讨论在费米能区下重离子碰撞的碎片产额分布是否可以作为研究轻核中$\alpha$团簇结构的工具。本文基于扩展的量子分子动力学输运模型(EMQD)模拟了16O具有4种不同的初始化$\alpha$构型(长链型、风筝型、四方型以及正四面体型)的16O+16O反应,通过观察碎片产额多重数分布情况研究了具有不同结构的团簇核的核反应。计算结果表明,碰撞后产生的自由质子及4He的产额受不同构型的影响明显,表明4He/proton可以作为团簇结构的一个表征量。此外,自由质子及4He的出射$\theta$和$\phi$角及动能能谱可以用来提取16O的$\alpha$团簇构型信息。     

New experimental measurement of natSe(n, γ) cross section between 1 eV to 1 keV at the CSNS Back-n facility

The ⁷⁴Se is one of 35 p-nuclei, and ⁸²Se is a r-process only nucleus, and their (n, γ) cross sections are vital input parameters for nuclear astrophysics reaction network calculations. The neutron capture cross section in the resonance range of isotopes and even natural selenium samples has not been measured. Prompt γ-rays originating from neutron-induced capture events were detected by four C₆D₆ liquid scintillator detectors at the Back-n facility of China Spallation Neutron Source (CSNS). The pulse height weighting technique (PHWT) was used to analyze the data in the 1 eV to 100 keV region. The deduced neutron capture cross section was compared with ENDF/B-VIII.0, JEFF-3.2, and JENDL-4.0, and some differences were found. Resonance parameters were extracted by the R-matrix code SAMMY in the 1 eV-1 keV region. All the cross sections of ^natSe and resonance parameters are given in the datasets. The datasets are openly available at http://www.doi.org/10.11922/sciencedb.j00113.00019.     

恒星氦燃烧关键反应12C(α,γ)16O天体物理S因子及其反应率

恒星氦燃烧阶段3α反应和12C（α,γ）16O反应相互竞争,两者的反应率共同决定了氦燃烧结束后12C与16O的丰度比,该比值是大质量恒星后继演化以及伴随的元素核合成过程的初始条件。目前,氦燃烧12C（α,γ）16O反应起始T₉=0.2处,天体物理模型要求的反应率的精确度要低于10%,然而尚未有实验或理论给出满足要求的结果。最为直接和可靠地获取12C（α,γ）16O反应率的方法,就是尽可能往低能区测量其天体物理S因子,然后通过理论外推到感兴趣的能区。为此基于经典的R-矩阵理论,建立了适用于低能核反应的多道、多能级的约化R-矩阵理论来拟合几乎所有可用的16O系统的实验数据。配合使用协方差统计和误差传播理论,拟合外推得到了客观的、内部自恰的和唯一性好的12C（α,γ）16O反应天体物理S因子。总的外推S因子STOT（0.3 MeV）=162.7±7.3 keV·b,理论上首次给出达到恒星演化与元素核合成模型的最低要求的S因子。基于计算给出的全能区的S因子,数值积分给出了温度位于0.04 6 T₉ 6 10的12C（α,γ）16O天体物理反应率。在T₉=0.2处,推荐的反应率为（7.83 ±0.35）×10-15 cm3mol-1s-1。During stellar helium burning, the rates of 3α and the 12C(α,γ)16O reaction, in competition with one another, determine the relative abundances of 12C and 16O in a massive star. The abundance ratio is the beginning condition of the following nucleosynthesis and star evolution of massive stars, which are extremely sensitive to the rate of 12C(α,γ)16O reaction at T₉=0.2. The most direct and trustworthy way to obtain the reaction rate of the 12C(α,γ)16O reaction is to measure the S factor for that reaction to as low energy as possible, and to extrapolate to energies of astrophysical interest. Based on a new multilevel and multichannel reduced R-matrix theory for applications in nuclear astrophysics, we have obtained an accurate and self-consistent astrophysical S factor of 12C(α,γ)16O, by a global fitting for almost all available experimental data of 16O system, with the coordination of covariance statistics and error-propagation theory. The extrapolated S factor of 12C(α,γ)16O was obtained with a recommended value STOT (0.3 MeV)=162.7±7.3 keV·b. And the reaction rates of 12C(α,γ)16O for stellar temperatures between 0.04 6 T₉ 6 10 are provided. At T₉=0.2, the reaction rate is (7.83 ±0.35)×10-15 cm3mol-1s-1, where stellar helium burning occurs.     

能量连续可调LCS光源SINAP-III

X/γ探测器在航天等国家战略需求领域具有非常广泛和重要的应用。 然而, X/γ探测器要在其有效能区进行精确的标定后才能发挥作用。 目前我国缺乏sub MeV～MeV能量连续可调、 单色性好的γ源, 而用于航天的X/γ探测器无法完成精确定标, 从而使航天探测的发展出现瓶颈问题。 提出了升级原有的激光康普顿散射(LCS)原理性实验装置的方案, 建立了一个通过改变激光入射角来连续调节散射光子能量、 准单色、 极化、 sub MeV～MeV LCS光源(SINAP-III), 从而开拓LCS光源在我国航天领域（如用于航天的X/γ探测器能量定标和抗辐射加固评估研究）的崭新应用前景, 并为将来建设一个基础和应用研究相结合的多功能的γ源实验平台打下基础。 The X/γ detectors in the field of national stratagem, such as astronautical technology, have very broad and important application. These detectors, however, will play their role properly only after accurate calibrations in effective energy region. For the shortage of continuously adjustable and quasi monochromatic γ source in China, it is impossible for the detector employed in aerospace to achieve an accurate calibration so that development of such detector has encountered a big obstacle (or a bottleneck). Therefore, we propose to upgrade the original LCS device to an adjustable photon energy by changing incident angle of laser beam, monochromatic, and polarized sub MeV~MeV LCS γ source(SIMAP III) , in order to explore the new applications of LCS γ source in aerospace as well as to establish a platform for a multifunctional of γ source.