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| 1 | Progress of Jinping Underground laboratory for Nuclear Astrophysics(JUNA)显示文摘Jinping Underground laboratory for Nuclear Astrophysics(JUNA) will take the advantage of the ultra-low background of CJPL lab and high current accelerator based on an ECR source and a highly sensitive detector to directly study for the first time a number of crucial reactions occurring at their relevant stellar energies during the evolution of hydrostatic stars. In its first phase, JUNA aims at the direct measurements of^(25)Mg(p,γ)^(26)Al,^(19)F(p,α)^(16)O,^(13)C(α,n)^(16)O and ^(12)C(α,γ)^(16)O reactions. The experimental setup,which includes an accelerator system with high stability and high intensity, a detector system, and a shielding material with low background, will be established during the above research. The current progress of JUNA will be given. | WeiPing Liu ZhiHong Li JiangJun He XiaoDong Tang Gang Lian Zhu An JianJun Chang Han Chen QingHao Chen XiongJun Chen ZhiJun Chen BaoQun Cui XianChao Du ChangBo Fu Lin Gan Bing Guo GuoZhu He Alexander Heger SuQing Hou HanXiong Huang Ning Huang BaoLu Jia LiYang Jiang Shigeru Kubono JianMin Li KuoAng Li Tao Li YunJu Li Maria Lugaro XiaoBing Luo HongYi Ma ShaoBo Ma DongMing Mei YongZhong Qian JiuChang Qin Jie Ren YangPing Shen Jun Su LiangTing Sun WanPeng Tan Isao Tanihata Shuo Wang Peng Wang YouBao Wang Qi Wu ShiWei Xu ShengQuan Yan LiTao Yang Yao Yang XiangQing Yu Qian Yue Sheng Zeng HuanYu Zhang Hui Zhang LiYong Zhang NingTao Zhang QiWei Zhang Tao Zhang XiaoPeng Zhang XueZhen Zhang ZiMing Zhang Wei Zhao Zuo Zhao Chao Zhou | 2016 | Science China(Physics,Mechanics & Astronomy)2016，59，4： | 3 |
| 2 | 2-10 Direct Measurement of the Main s-process Neutron Source显示文摘The 13C(, n)16O reaction is the key neutron source reaction for the main s-process nucleosynthesis[1]. Theimportant energy range (Gamow window) for the 13C( , n)16O reaction during the s-process spans from 140 to230 keV in the center of mass frame. Because of the Coulomb barrier, the cross sections drop exponentially asmeasurement approaches the Gamow window energies. Limited by cosmic ray background and the available beamintensity, the ground-based measurements are limited to energies above 280 keV. Therefore, the extrapolationbased on R-matrix calculation and/or in-direct measurement is the current method to estimate the cross sectionsfor astrophysical interest with limited precision. Moreover, due to the existence of sub-threshold resonances, thereare rather large uncertainties associated with the extrapolated cross sections which limit the precision of the currentreaction rate and thus prevent us from a complete understanding of the nucleosynthesis of heavy elements. | Tang Xiaodong Ren Jie Chen Han Chen Zhijun Chen Xiongjun Huang Hanxiong Jiang Liyang Li Kuoang Ruan Xuchao Wang Shuo Zhang Ningtao the JUNA collaboration | 2014 | IMP & HIRFL Annual Report2014，，1： | 0 |
| 3 | 2-11 Stellar -decay Rate of 59Fe and Its Impact on the 60Fe Nucleosynthesis显示文摘60Fe is a long-lived nucleus (T1=2=2.62×106 a) which is mainly synthesized in the Carbon-shell burning ofmassive stars. It still could be observed nowadays after being ejected to the space after massive star ends its life assupernova. Along with another long-lived nucleus 26Al (T1=2=7.17×105 a) which is synthesized in the similar stars,the observation of their decay could provide the information of stellar evolution. From 2002-2005 the INTEGRALsatellite with detector obtained 60Fe/26Al flux ratio in our Galaxy to be 0.148(60)[1]. It's significantly smallerthan the theoretical prediction 0.45[2], and indicated that the theory need to be improved to increase the 60Fe yieldor decrease 26Al yield. 60Fe is produced by neutron capture reactions: 58Fe(n, )59Fe and 59Fe(n, )60Fe. Thecompetition between -decay of 59Fe and its neutron capture plays an important role in 60Fe synthesis path. In thepresent work, the impact on the 60Fe synthesis of the -decay process in stellar environment is studied. | Li Kuoang Lam Yihua Qi Chong Tang Xiaodong Zhang Ningtao | 2014 | IMP & HIRFL Annual Report2014，，1： | 0 |
| 4 | Determination of the cluster spectroscopic factor of the 10.3 MeV state in ^(12)Be显示文摘From an inelastic excitation and breakup experiment with a12Be beam at 29 MeV/u,a large4He+8He cluster decay width of 1.1(2)MeV is determined for a state at an excitation energy of 10.3 MeV and with a spin parity of 0+.By using the R-matrix analysis,a cluster spectroscopic factor of 0.53(10)is extracted from the cluster partial width,providing a strong support for the clustering structure in12Be.A specially designed zero-degree telescope played an essential role in the present experiment and has been demonstrated to be a promising tool in future studies of the molecular-like resonances near the cluster separation threshold. | YANG ZaiHong YE YanLin LI ZhiHuan LOU JianLin XU FuRong PEI JunCheng TIAN ZhengYang LI KuoAng SUN YeLei CHEN Jie LI Jing JIANG Wei YANG Biao CHEN SiDong LIU Qiang ZANG HongLiang FENG Jun YIN ZheWei | 2014 | Science China(Physics,Mechanics & Astronomy)2014，57，9： | 0 |
| 5 | 通过^(1)H(^(15)O,p)^(15)O弹性散射来研究^(16)F的能级性质显示文摘The understanding of open quantum systems in unbound nuclei is a challenge to the nuclear structure research[1].The continuum coupling effect may lead to a reordering of the shells in such systems[2].A way to study this effect is to compare the level schemes of two mirror nuclei involving an unbound and a bound nucleus such as 16F and 16N[3].Here we report an experiment of studying the level properties of 16F using the resonant elastic scattering with an 15O radioactive beam delivered by the Radioactive Ion Beam Line at Lanzhou(RIBLL)[4]. | Ru Longhui Hu Jun Liu Enqiang Bai Zhen Duan Fangfang Fang Xiao Hou Suqing Hu Qiang Ji Liancheng Jin Shuya Li Kuoang Li Yiyang Li Ruojie Ma Peng Ma Junbing Sun Xinxin Shi Guozhu Tang Xiaodong Wang Xinyu Wang Jiansong Wang Yufeng Wu Jiatong Xu Xiaodong Xu Shiwei Xin Wenyu Yang Kaiping Yang Yanyun NMichel | 2018 | IMP & HIRFL Annual Report2018，，1： | 0 |
| 6 | Fusion Studies with Low-intensity Beams Using the Active Target Time Projection Chamber显示文摘Fusion reactions play a very important role for the creation of heavier elements in the quiescent and explosive burning phases in stars.Fusion processes also generate the energy in the Sun that created and maintain life in our earth[1]. | Zhang Ningtao Zhang Zhichao Zhang Jinlong Tang Xiaodong Lu Chengui Gao Bingshui Li Yutian Li Kuoang Pu Tianlei Ru Longhui Wang Xinyu Xu Xiaodong Cai Ziwei Li Qite Ji Binfei Xu Jinyan | 2019 | IMP & HIRFL Annual Report2019，，1： | 0 |
| 7 | 2-7 Study of Zr-Nb Cycle in Astrophysical rp-process显示文摘At a certain high temperature,this cycle will be dominant and end the rp-process to heavier region[2].It provides an upper temperature limit for rp-process along the proton drip line to produce nuclides beyond A=84,including the light p nuclides of 92;94Mo,96;94Ru.The existence of Zr-Nb cycle is an important question in rp-process[2].α-separation energy(Sα)of 84Mo plays an important role in the formation of this cycle.A strong enhancement of 83Nb(p,α)reaction rate is due to a very low Sαof 84Mo[1]. | Xing Yuanming Zhang Yuhu Wang Meng Li Kuoang Tang Xiaodong Xu Hushan Chen Ruijiu Chen Xiangcheng Fu Chaoyi Ge Zhuang Gao Bingshui Huang Wenjia Ma Xinwen Mao Ruishi S.A.Litvinov Shuai Peng Tu Xiaolin Xiao Guoqing Xu Xing Yan Xinliang Yu.A.Litvinov Yang Jiancheng Yuan Youjin Zhang Wei Zeng Qi Zhou Xiaohong | 2016 | IMP & HIRFL Annual Report2016，，1： | 0 |
| 8 | 2-11 Stellarβ-decay Rate of 134Cs显示文摘134Cs a branching point in s-process path which is shown in Fig.1.The branching ratio is defined as fβ=λβ/(λβ+λn).It could be deduced from the abundance of 134Ba and 136Ba since 136Ba goes through both decay and neutroncapture of 134Cs while 134Ba only experiences decay channel[1].Due to both 134Ba and 134Ba are pure s-process nuclei,this branching point is a good approach to determine the s-process parameters.With temperaturedependentβ-decay rate of 134Cs,the temperature of s-process could be deduced. | Li Kuoang Qi Chong Tang Xiaodong | 2016 | IMP & HIRFL Annual Report2016，，1： | 0 |
| 9 | 2-15 16O+40Ar Experiment Using TPC at RIBLL1显示文摘It has been proposed that fusion reactions between neutron-rich light nuclei,for example 24C,24O and 28Ne,may contribute to achieving the ignition temperature for explosive carbon burning process during superbusrsts[1,2].Studies of fusion reactions involving neutron-rich nuclei are beyond ordinary experimental techniques,since the intensity of radioactive beam become low for these measurements[3].The active target technique using TPC(Time Projection Chamber),with properties of multi-sampling,high efficiency and low background,is a suitable solution to the problem. | Zhang Ningtao Lu Chengui Ji Liancheng Chen Han Chen Zhijun Hu Jun Li Kuoang Ma Shaobo Ru Longhui Tang Xiaodong Xu Shiwei | 2016 | IMP & HIRFL Annual Report2016，，1： | 0 |
| 10 | 2-16 Experimental Study of 13N(α,p)16O at the Stellar Energies显示文摘The presolar SiC grains[1]carry the original stellar nucleosynthesis signature.Their isotopic anomalies compared to the sun are the strong constrains in the supernovae(SN)model calculations.The 15N-excess in some SiC-AB grains(12C/13C<10 and 14N/15N<272)is one of the challenges of core-collapse supernovae(CCSNe)models[2].Recently,Pignatari pointed out that the entrainment of H-rich material into the He shell before the SN explosion allows the coproduction of 13C,15N and 26Al,which provides a new production scenario for SiC-AB grains[2].In the He shell nucleosynthesis,the 13C is produced through 12C(p,γ)13N(β+γ)13C reaction.The 14N is synthesized through 13N(n,γ)and 13C(p,γ)reactions. | Lin Weiping Ma Shaobo Hu Jun Bai Zhen Chen Han Chen Zhijun Duan Fangfang Gao Bingshui Gao Zhihao Hou Suqing Ji Liancheng Jia Baolu Jiao Lei Jin ShuYa Liu Xingquan Li Kuoang Lu Tan Ma Junbing Ma Peng Tang Xiaodong Wang Xinyu Xu Shiwei Yang Yanyun Yu Gongming Yu Xiangqing Zhai Yaojie Zhang Ningtao Zhang Xing | 2016 | IMP & HIRFL Annual Report2016，，1： | 0 |
| 11 | 2-7 Voltage Calibration and Energy Spread Measurement of 320 kV Platform at the Institute of Modern Physics显示文摘Four key reactions, 12C(, )13O, 13C(, n)16O, 25Mg(p, )26Al and 19F(p, )16O, will be studied for the first time within or near the astrophysical relevant energy regions (Gamow window) at Jinping Underground laboratory for Nuclear Astrophysics (JUNA)[1], which will take the advantage of the ultra-low background of China JinPing underground Laboratory (CJPL), high current accelerator based on ECR source and a highly sensitive detection system. | Wang Shuo Li Kuoang Xu Shiwei Ma Shaobo Tang Xiaodong Zhang Ningtao Su Jun Shen Yangping Chen Han Chen Zhijun Pei Changjin Zhu Hao Zhang Zirui Zhang Naibo Wang Shouyu | 2015 | IMP & HIRFL Annual Report2015，，1： | 0 |
| 12 | A method for determination of deuterium impurity in the helium beam显示文摘Both the LUNA(Laboratory for Underground Nuclear Astrophysics)collaboration in Europe and the JUNA(Jinping Underground Laboratory for Nuclear Astrophysics)collaboration in China are planning to study the key reactions during the stellar helium burning at or close to their stellar energies in deep underground laboratories[1-3].The success of such experiments relies on the ratio of the reaction | Han Chen ShiWei Xu NingTao Zhang Jun Hu KuoAng Li ShaoBo Ma XiChao Ruan XiaoDong Tang LiYong Zhang | 2018 | Science China(Physics,Mechanics & Astronomy)2018，61，5： | 0 |
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