Silver indium cadmium(Ag–In–Cd) control rod is widely used in pressurized water reactor nuclear power plants,and it is continuously consumed in a high neutron flux environment. The mass ratio of ^(107)Ag in the Ag...Silver indium cadmium(Ag–In–Cd) control rod is widely used in pressurized water reactor nuclear power plants,and it is continuously consumed in a high neutron flux environment. The mass ratio of ^(107)Ag in the Ag–In–Cd control rod is 41.44%. To accurately calculate the consumption value of the control rod, a reliable neutron reaction cross section of the ^(107)Ag is required. Meanwhile,^(107)Ag is also an important weak r nucleus. Thus, the cross sections for neutron induced interactions with ^(107)Ag are very important both in nuclear energy and nuclear astrophysics. The(n, γ) cross section of ^(107)Ag has been measured in the energy range of 1–60 eV using a back streaming white neutron beam line at China spallation neutron source. The resonance parameters are extracted by an R-matrix code. All the cross section of ^(107)Ag and resonance parameters are given in this paper as datasets. The datasets are openly available at http://www.doi.org/10.11922/sciencedb.j00113.00010.展开更多
The^(74)Se is one of 35 p-nuclei,and^(82)Se 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...The^(74)Se is one of 35 p-nuclei,and^(82)Se 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.Promptγ-rays originating from neutron-induced capture events were detected by four C_(6)D_(6) 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 e V to 100 ke V 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 e V-1 ke V region.All the cross sections ofnatSe and resonance parameters are given in the datasets.The datasets are openly available at http://www.doi.org/10.11922/sciencedb.j00113.00019.展开更多
The ambiguity of the structure of ^(12)Be especially in the configuration of Be ground state has attracted a lot of attention recently.We notice that the nuclear reaction cross section or at low energy region is sensi...The ambiguity of the structure of ^(12)Be especially in the configuration of Be ground state has attracted a lot of attention recently.We notice that the nuclear reaction cross section or at low energy region is sensitive to the surface structure of ^(12)Be,which is greatly impacted by the ground state configuration of ^(12)Be especially by the occupancy probability of the s orbital component.By using existed interaction cross section data of ^(12)Be on C at 790 MeV/nucleon and Glauber model,the upper limit of the s orbital occupation probability of ^(12)Be ground state is roughly determined to be about 56%with Single Particle Model calculations.This demonstrates that the method is very promising to determine the s orbital component of ^(12)Be with proper nuclear-matter density distribution calculations for different orbitals of ^(12)Be ground state.Hence we bring forward to determine the s orbital component of ^(12)Be by measuring the ctr of ^(12)Be on C and Al at several tens of MeV/nucleon.In this paper,the feasibility and detailed experimental scheme of the ctr measurement are carefully studied.The precision of the s orbital occupation probability of ^(12)Be ground state is expected to achieve 9%by using the proposed 2%ctr data.展开更多
The astrophysical reaction rate of 12C（α,γ）16O plays a key role in massive star evolution. However, this reaction rate and its uncertainties have not been well determined yet, especially at T9=0.2. The existing re...The astrophysical reaction rate of 12C（α,γ）16O plays a key role in massive star evolution. However, this reaction rate and its uncertainties have not been well determined yet, especially at T9=0.2. The existing results even disagree with each other to a certain extent. In this paper, the El, E2 and total （E1＋E2） 12C（α,γ）16O reaction rates are calculated in the temperature range from T9=0.3 to 2 according to all the available cross section data. A new analytic expression of the 12C（α,γ）16O reaction rate is brought forward based on the reaction mechanism. In this expression, each part embodies the underlying physics of the reaction. Unlike previous works, some physical parameters are chosen from experimental results directly, instead of all the parameters obtained from fitting. These parameters in the new expression, with their 3σ fit errors, are obtained from fit to our calculated reaction rate from T9=0.3 to 2. Using the fit results, the analytic expression of 12C（α,γ）16Oreaction rate is extrapolated down to T9=0.05 based on the underlying physics. The 12C（α,γ）16O reaction rate at T9=0.2 is （8.78 ± 1.52） × 10^15 cm3s^-1mol^-1. Some comparisons and discussions about our new 12C（α,γ）16Oreaction rate are presented, and the contributions of the reaction rate correspond to the different part of reaction mechanism are given. The agreements of the reaction rate below T9=2 between our results and previous works indicate that our results are reliable, and they could be included in the astrophysical reaction rate network. Furthermore, we believe our method to investigate the 12C（α,γ）16O reaction rate is reasonable, and this method can also be employed to study the reaction rate of other astrophysical reactions. Finally, a new constraint of the supernovae production factor of some isotopes are illustrated according to our 12C（α,γ）16O reaction rates.展开更多
平坦效率对于实现光中子反应的单中子、双中子和三中子事件的区分和截面的计算非常关键。介绍了一种用于逆康普顿散射γ源(Shanghai Laser Electron Gamma Source,SLEGS)光中子(γ,n)截面测量的4π平坦效率3He中子探测器阵列的设计与模...平坦效率对于实现光中子反应的单中子、双中子和三中子事件的区分和截面的计算非常关键。介绍了一种用于逆康普顿散射γ源(Shanghai Laser Electron Gamma Source,SLEGS)光中子(γ,n)截面测量的4π平坦效率3He中子探测器阵列的设计与模拟。采用Geant4程序对平坦效率3He探测器的优化布局和效率进行了模拟,针对设计的由20只Φ50 mm×500 mm 5 cm 3He正比计数管和6只Φ25 mm×500 mm 3He正比计数管组成的4π平坦效率中子探测器,模拟给出探测器平均效率曲线在1 keV^6 MeV的效率为34.4%~45.9%。模拟中以209Bi靶为例,靶尺寸为Φ20 mm×4 mm,通过对产生中子的角分布,能谱的模拟计算,发现中子出射角度在90°对称,探测器的4π布局能够完全覆盖入射到聚乙烯慢化体的中子,出射中子能量随着中子分离能呈现出规律的变化关系;随着γ能量增加,出射道开放增多,出射中子的能量总是分布在1 keV^4 MeV之间,探测器阵列在这一能区的平均效率为40%~46%。展开更多
恒星氦燃烧阶段3α反应和^(12)C(α,γ)^(16)O反应相互竞争,两者的反应率共同决定了氦燃烧结束后^(12)C与^(16)O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^(12)C(α,γ)^(16)O反应起始T_9=...恒星氦燃烧阶段3α反应和^(12)C(α,γ)^(16)O反应相互竞争,两者的反应率共同决定了氦燃烧结束后^(12)C与^(16)O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^(12)C(α,γ)^(16)O反应起始T_9=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^(12)C(α,γ)^(16)O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^(16)O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^(12)C(α,γ)^(16)O反应天体物理S因子。总的外推S因子STOT(0.3 Me V)=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≤T_9≤10的^(12)C(α,γ)^(16)O天体物理反应率。在T_9=0.2处,推荐的反应率为(7.83±0.35)×10^(-15)cm^3mol^(-1)s^(-1)。展开更多
Based on the facility of the Shanghai Laser Electron Gamma Source （SLEGS）, the transmutation for nuclear wastes such as 137^Cs and 129^I is investigated. It is found that nuclear waste can be transmuted efficiently ...Based on the facility of the Shanghai Laser Electron Gamma Source （SLEGS）, the transmutation for nuclear wastes such as 137^Cs and 129^I is investigated. It is found that nuclear waste can be transmuted efficiently via photonuclear reaction triggered by gamma photons generated from Compton backscattering between CO2 laser photons and 3.5 GeV electrons. The nuclear activities of 137^Cs and 129^I are evaluated and compared with the results of transmutation triggered by bremsstrahlung gamma photons driven by ultra intense laser. Due to the better character of gamma photon spectrum as well as the high brightness of gamma photons, the transmutation rate of Compton backscattering method is much higher than that of the bremsstrahlung method.展开更多
The measurement of parity-violating （PV） observables in few-nucleon system can shed light on our current understanding of the weak interaction between nucleons.Theoretical models describe the nucleonnucleon weak int...The measurement of parity-violating （PV） observables in few-nucleon system can shed light on our current understanding of the weak interaction between nucleons.Theoretical models describe the nucleonnucleon weak interaction at low energies use a series of undetermined parameters.Two parity violating measurements have been considered： the capture of polarized slow neutrons on hydrogen （n ＋ p → d ＋ γ） at Los Alamos National Laboratory for first phase and Oka Ridge National Laboratory for second phase and the helicity dependence of the deuteron photodisintegration cross section using circularly polarized photons （γ ＋ d → n ＋ p） at Shanghai Institute of Applied Physics.The goal of both experiments is to constraint the weak meson-nucleon couplings to a precision of 1 ×10^-8 .The introduction of both experiments is presented.展开更多
The dark matter puzzle is one of the most important fundamental physics questions in the 21st century.There is no doubt that solving the puzzle will be a new milestone for human beings in achieving a deeper understand...The dark matter puzzle is one of the most important fundamental physics questions in the 21st century.There is no doubt that solving the puzzle will be a new milestone for human beings in achieving a deeper understanding of nature.Herein,we propose the use of the Shanghai laser electron gamma source(SLEGS)to search for dark matter candidate particles,including dark pseudoscalar particles,dark scalar particles,and dark photons.Our simulations indicate that,with some upgrading,electron facilities such as SLEGS could be competitive platforms in the search for light dark matter particles with a mass below tens of keV.展开更多
基金supported by the National Natural Science Foundation of China (Grant Nos. 11875311, 11905274, 1705156, U2032146, 11865010, 11765015, and 1160509)the Natural Science Foundation of Inner Mongolia, China (Grant Nos. 2019JQ01 and 2018MS01009)the Strategic Priority Research Program of the Chinese Academy of Sciences (Grant No. XDB34030000)。
文摘Silver indium cadmium(Ag–In–Cd) control rod is widely used in pressurized water reactor nuclear power plants,and it is continuously consumed in a high neutron flux environment. The mass ratio of ^(107)Ag in the Ag–In–Cd control rod is 41.44%. To accurately calculate the consumption value of the control rod, a reliable neutron reaction cross section of the ^(107)Ag is required. Meanwhile,^(107)Ag is also an important weak r nucleus. Thus, the cross sections for neutron induced interactions with ^(107)Ag are very important both in nuclear energy and nuclear astrophysics. The(n, γ) cross section of ^(107)Ag has been measured in the energy range of 1–60 eV using a back streaming white neutron beam line at China spallation neutron source. The resonance parameters are extracted by an R-matrix code. All the cross section of ^(107)Ag and resonance parameters are given in this paper as datasets. The datasets are openly available at http://www.doi.org/10.11922/sciencedb.j00113.00010.
基金supported by the National Natural Science Foundation of China(Grant Nos.11875311,11905274,11705156,11605097,and U2032146)the Strategic Priority Research Program of Chinese Academy of Sciences(Grant No.XDB34030000)。
文摘The^(74)Se is one of 35 p-nuclei,and^(82)Se 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.Promptγ-rays originating from neutron-induced capture events were detected by four C_(6)D_(6) 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 e V to 100 ke V 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 e V-1 ke V region.All the cross sections ofnatSe and resonance parameters are given in the datasets.The datasets are openly available at http://www.doi.org/10.11922/sciencedb.j00113.00019.
基金Supported by the National Natural Science Foundation of China(No.11179018 and 11305238)the Instrument Developing Project of the Chinese Academy of Sciences(No.YZ201246)
文摘The ambiguity of the structure of ^(12)Be especially in the configuration of Be ground state has attracted a lot of attention recently.We notice that the nuclear reaction cross section or at low energy region is sensitive to the surface structure of ^(12)Be,which is greatly impacted by the ground state configuration of ^(12)Be especially by the occupancy probability of the s orbital component.By using existed interaction cross section data of ^(12)Be on C at 790 MeV/nucleon and Glauber model,the upper limit of the s orbital occupation probability of ^(12)Be ground state is roughly determined to be about 56%with Single Particle Model calculations.This demonstrates that the method is very promising to determine the s orbital component of ^(12)Be with proper nuclear-matter density distribution calculations for different orbitals of ^(12)Be ground state.Hence we bring forward to determine the s orbital component of ^(12)Be by measuring the ctr of ^(12)Be on C and Al at several tens of MeV/nucleon.In this paper,the feasibility and detailed experimental scheme of the ctr measurement are carefully studied.The precision of the s orbital occupation probability of ^(12)Be ground state is expected to achieve 9%by using the proposed 2%ctr data.
基金Supported by the National Natural Science Foundation of China under Grant Nos 10675149 and 10535010, the Chinese Academy of Sciences under Grant No KJCX3.SYW.N1, and the National Basic Research Programme of China under Grant No 2007CB81500. We thank Wang Shunjin for his suggestion and fruitful discussion.
基金Project supported partially by the Innovation Program of Science and Technology of the Chinese Academy of Sciences (Grant Nos KJCX2.SW.N13 and KJCX3.SYW.N2)the National Natural Science Foundation of China (Grant Nos 10775167, 10675156 and 10610285)+2 种基金the Major State Basic Research Development Program (Grant No 2007CB815004)the Hundred Talent Project of the Chinese Academy of Sciences (Grant No 26010701)the Shanghai Development Foundation for Science and Technology (Grant No 06JC14082)
文摘The astrophysical reaction rate of 12C（α,γ）16O plays a key role in massive star evolution. However, this reaction rate and its uncertainties have not been well determined yet, especially at T9=0.2. The existing results even disagree with each other to a certain extent. In this paper, the El, E2 and total （E1＋E2） 12C（α,γ）16O reaction rates are calculated in the temperature range from T9=0.3 to 2 according to all the available cross section data. A new analytic expression of the 12C（α,γ）16O reaction rate is brought forward based on the reaction mechanism. In this expression, each part embodies the underlying physics of the reaction. Unlike previous works, some physical parameters are chosen from experimental results directly, instead of all the parameters obtained from fitting. These parameters in the new expression, with their 3σ fit errors, are obtained from fit to our calculated reaction rate from T9=0.3 to 2. Using the fit results, the analytic expression of 12C（α,γ）16Oreaction rate is extrapolated down to T9=0.05 based on the underlying physics. The 12C（α,γ）16O reaction rate at T9=0.2 is （8.78 ± 1.52） × 10^15 cm3s^-1mol^-1. Some comparisons and discussions about our new 12C（α,γ）16Oreaction rate are presented, and the contributions of the reaction rate correspond to the different part of reaction mechanism are given. The agreements of the reaction rate below T9=2 between our results and previous works indicate that our results are reliable, and they could be included in the astrophysical reaction rate network. Furthermore, we believe our method to investigate the 12C（α,γ）16O reaction rate is reasonable, and this method can also be employed to study the reaction rate of other astrophysical reactions. Finally, a new constraint of the supernovae production factor of some isotopes are illustrated according to our 12C（α,γ）16O reaction rates.
文摘平坦效率对于实现光中子反应的单中子、双中子和三中子事件的区分和截面的计算非常关键。介绍了一种用于逆康普顿散射γ源(Shanghai Laser Electron Gamma Source,SLEGS)光中子(γ,n)截面测量的4π平坦效率3He中子探测器阵列的设计与模拟。采用Geant4程序对平坦效率3He探测器的优化布局和效率进行了模拟,针对设计的由20只Φ50 mm×500 mm 5 cm 3He正比计数管和6只Φ25 mm×500 mm 3He正比计数管组成的4π平坦效率中子探测器,模拟给出探测器平均效率曲线在1 keV^6 MeV的效率为34.4%~45.9%。模拟中以209Bi靶为例,靶尺寸为Φ20 mm×4 mm,通过对产生中子的角分布,能谱的模拟计算,发现中子出射角度在90°对称,探测器的4π布局能够完全覆盖入射到聚乙烯慢化体的中子,出射中子能量随着中子分离能呈现出规律的变化关系;随着γ能量增加,出射道开放增多,出射中子的能量总是分布在1 keV^4 MeV之间,探测器阵列在这一能区的平均效率为40%~46%。
文摘恒星氦燃烧阶段3α反应和^(12)C(α,γ)^(16)O反应相互竞争,两者的反应率共同决定了氦燃烧结束后^(12)C与^(16)O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^(12)C(α,γ)^(16)O反应起始T_9=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^(12)C(α,γ)^(16)O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^(16)O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^(12)C(α,γ)^(16)O反应天体物理S因子。总的外推S因子STOT(0.3 Me V)=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≤T_9≤10的^(12)C(α,γ)^(16)O天体物理反应率。在T_9=0.2处,推荐的反应率为(7.83±0.35)×10^(-15)cm^3mol^(-1)s^(-1)。
基金Knowledge Innovation Project of Chinese Academy of Sciences (KJCX2-SW-N13)China Postdoctoral ScienceFoundation, National Natural Science Foundation of China (10475108, 10605036, 10405032)+1 种基金One Hundred Person Project of SINAPShanghai Development Foundation for Science and Technology (06QA14062)
文摘Based on the facility of the Shanghai Laser Electron Gamma Source （SLEGS）, the transmutation for nuclear wastes such as 137^Cs and 129^I is investigated. It is found that nuclear waste can be transmuted efficiently via photonuclear reaction triggered by gamma photons generated from Compton backscattering between CO2 laser photons and 3.5 GeV electrons. The nuclear activities of 137^Cs and 129^I are evaluated and compared with the results of transmutation triggered by bremsstrahlung gamma photons driven by ultra intense laser. Due to the better character of gamma photon spectrum as well as the high brightness of gamma photons, the transmutation rate of Compton backscattering method is much higher than that of the bremsstrahlung method.
基金Supported by One Hundred Person Project of Chinese Academy of Sciences (26010701)Knowledge Innovation Project of the Chinese Academy of Sciences (KJCX2-SW-N13)+1 种基金Pujiang Talent Project of the Shanghai Science and Technology Committee (06PJ14114)National Natural Science Foundation of China (10675156)
文摘The measurement of parity-violating （PV） observables in few-nucleon system can shed light on our current understanding of the weak interaction between nucleons.Theoretical models describe the nucleonnucleon weak interaction at low energies use a series of undetermined parameters.Two parity violating measurements have been considered： the capture of polarized slow neutrons on hydrogen （n ＋ p → d ＋ γ） at Los Alamos National Laboratory for first phase and Oka Ridge National Laboratory for second phase and the helicity dependence of the deuteron photodisintegration cross section using circularly polarized photons （γ ＋ d → n ＋ p） at Shanghai Institute of Applied Physics.The goal of both experiments is to constraint the weak meson-nucleon couplings to a precision of 1 ×10^-8 .The introduction of both experiments is presented.
基金Supported by the National Nature Science Foundation of China(11875191,11775140)the Strategic Priority Research Program(CAS XDB1602)。
文摘The dark matter puzzle is one of the most important fundamental physics questions in the 21st century.There is no doubt that solving the puzzle will be a new milestone for human beings in achieving a deeper understanding of nature.Herein,we propose the use of the Shanghai laser electron gamma source(SLEGS)to search for dark matter candidate particles,including dark pseudoscalar particles,dark scalar particles,and dark photons.Our simulations indicate that,with some upgrading,electron facilities such as SLEGS could be competitive platforms in the search for light dark matter particles with a mass below tens of keV.
