Indirect Measurement of Cross Section of ~9Be(p,α)~6Li

The cross section of 9Be(p,α)6Li at low energies is important for nuclear astrophysics. But it is difficult for direct measurement because of the Coulomb barrier and electron screening effect. In order to measure the 9Be(p,α)6Li bare nucleus cross secti…     

Theoretical Study of ^2H（d,γ）^4He Reaction Below Ecm〈3 MeV

The reaction cross sections of ^2H（d,γ）^4He at the astrophysically interesting energies （about below few hundreds of keV） are extremely low. Presently it is impractical to measure in the laboratory. Therefore the theoretical investigation is required to predict the relevant cross section data.     

Indirect Measurement of Astrophysical S(E) Factor for ~9Be(p,α)~6Li Reaction by Means of the Trojan Horse Method

The beryllium abundance acts as a key role for understanding the inhomogeneous Big Bang nucleosynthesis. In order to measure the 9Be(p, α)6Li bare nucleus cross section and S(E) factor at astrophysical energies, the Trojan Horse Method (THM) can be appli…     

The cross section calculation of ~(112)Sn(α,γ) ~(116)Te reaction with different nuclear models at the astrophysical energy range

The theoretical cross section calculations for the astrophysical p process are needed because most of the related reactions are technically very difficult to be measured in the laboratory. Even if the reaction was measured,most of the measured reactions have been carried out at the higher energy range from the astrophysical energies.Therefore, almost all cross sections needed for p process simulation have to be theoretically calculated or extrapolated to the astrophysical energies.~(112)Sn(α,γ)~(116)Te is an important reaction for the p process nucleosynthesis. The theoretical cross section of ~(112)Sn(α,γ)~(116)Te reaction was investigated for different global optical model potentials,level density, and strength function models at the astrophysically interested energies. Astrophysical S factors were calculated and compared with experimental data available in the EXFOR database. The calculation with the optical model potential of the dispersive model by Demetriou et al., and the back-shifted Fermi gas level density model and Brink-Axel Lorentzian strength function model best served to reproduce experimental results at an astrophysically relevant energy region. The reaction rates were calculated with these model parameters at the p process temperature and compared with the current version of the reaction rate library Reaclib and Starlib.     

Activation cross section measurement for ^165Ho（n,γ）^166m Ho and ^151Eu（n,γ）^152g Eu

The cross sections for ^151Eu(n,γ）152gEu reaction in the neutron energy range of 22-1100keV and the cross sections for ^165Ho(n,γ)166m Ho reaction at the neutron energies of 203.676 and 974keV are measured by activation method.The data of the neutron activation cross section at given energy ranges for ^165Ho and ^151Eu are presented for the first time.     

Measurements of fast—neutron capture cross sections for ^159Tb and ^169Tm

The neutron capture cross sections for ^159Tb and ^169Tm relative to the ^197Au (n,γ)^198Au reaction are measured at neutron energies of 0.57,1.10 and 1.60 MeV by using the activation method.The activities of the products are measured with a high resolution HPGe detector gamma-ray spectrometer.The errors of the present work are 5-6% for Tb,6-7% for Tm.The recommended data in energy region of 0.4-3.0MeV are given as compared with other data published previously.     

Measurement of Branching Ration of Deuterium Induced Reactions on ^2He at 20 keV

Nuclear reactions between light charged particles at low energy play important role in many areas of basic and applied physics. However due to the cross section drops dramatically with the decrease of incident energy, the measurement of the ^2He（d,γ）^4He reaction has to be conducted with very low effect     

Determination of Astrophysical ^26Si（p, γ）^27p Reaction Rate From Asymptotic Normalization Coefficients of ^27Mg →^26Mg ＋ n

The 1.809 MeV T-ray from the decay of ^26Al is an excellent observable for some astrophysical events, such as novae and X-ray burst. The nucleosynthesis of ^26A1 is dominated by the reaction chain ^24Mg（p,γ）^25Al（β＋）^25Mg（p,γ）^26Al, however,     

Unusual Threshold Anomaly in ^6Li＋^208Pb System

The angular distributions of elastic scattering for ^6Li＋^208Pb system have been measured at several energies around the Coulomb barrier. The parameters of optical potential are extracted by means of a phenomenological optical model analysis. It is found that the real and imaginal potentials show a pronounced energy dependence.     

Indirect Measurement of Astrophysical ~(13)C(α,n)~(16)O S-Factors

The 13C(α,n)16O reaction is believed to be the main neutron source reaction for the s-process in asymptotic giant branch (AGB) stars. The astrophysical S-factors of this reaction have been determined based on an evaluation of the α spectroscopic factor of the 1/2+ subthreshold state in 17O (Ex=6.356 MeV) by using the 13C(11B,7Li)17O α transfer reaction. Our result confirms that the 1/2+ subthreshold resonance is dominant for the 13C(α,n)16O reaction at low energies of astrophysical interest.     

Analysis and Prediction of the Cross Sections of d ~6Li and d ~7Be Reactions for Energy up to 30 MeV

A set of deuteron optical potential parameters is obtained based on the relevant experimental data, and various nuclear data of d ~6Li reaction at incident energies spanning 0.1～30 MeV were calculated with the Distorted Wave Born Approximation, preequilibrium nuclear reaction and Hauser-Feshbach (HF) theory.The cross sections of d ~7Be reaction were predicted. The results show that the experimental measure- ment for d ~7Be reaction is feasible at HI-13 tandem accelerator.     

Astrophysical 13N（p, γ）14O Reaction Rate

13N（p, γ）14O is is one of the key reactions in the hot CNO cycle which occurs at stellar temperatures around T9≤0.1. At the energies of astrophysical interest, the 13N（p, γ）14O reaction is dominated by the low energy tail of the s-wave capture on the broad 1- resonance at Er = 527.9 keV （which has a total width of （37.34-0.9） keV）. A considerable effort has been expended in recent years to determine the parameters for the resonance. These include the direct measurements using the radioactive ^13N beam, particle transfer reactions, and coulomb dissociation of high-energy ^14O beams in the field of a heavy nucleus.     

Determination of the Astrophysically Relevant ~6Li(n,γ)~7Li Cross Sections from the ~7Li(~6Li,~7Li)~6Li Elastic-Transfer Reaction

Angular distributions for the ~7(Li)(~6(Li),~7(Li))~6(Li) Li elastic-transfer reaction have been measured with the Q3D magnetic spectrograph at the HI-13 tandem accelerator of Beijing, China. The neutron spectroscopic factors of 7Li are derived by comparing the calculated differential cross sections, which are obtained through the distorted-wave Born approximation (DWBA) calculation, to the experimental data. And these spectroscopic factors are then used to deduce the direct capture cross sections in 6Li(n,γ)7 Li at energies of astrophysical relevance.     

Applications of Skyrme Energy-Density Functional to Fusion Reactions for Synthesis of Superheavy Nuclei

It is of great importance to predict fusion cross sections and to analyze reaction mechanism for massive heavy-ion fusion reactions, especially for fusion reactions leading to superheavy nuclei. In those reactions, the calculation of the capture cross section is of crucial importance. It is known that Wong＇s formula based on one-dimensional barrier penetration can describe the fusion excitation function well for light reaction systems, while it fails to give satisfying results for heavy reaction systems at energies near and below the barrier. For solving this problem, we applied the Skyrme energy-density functional for the first time to study heavy-ion fusion reactions. The barrier for fusion reaction was calculated by the Skyrme energy-density functional together with the semi-classical extended Thomas-Fermi method.     

Further Analysis of Neutron Double-Differential Cross Section of n＋^16O at 14.1 and 18 MeV

By using a new reaction model for light nuclei, the double-differential cross section of total outgoing neutron with LUNF code for n＋^16O reactions at En=14.1 MeV and 18 MeV have been calculated and analyzed. The opened reaction channels, which have contribution to emit the neutrons, are listed in detail. To improve the fitting results the direct inelastic scattering mechanism is involved. The calculated results agree fairly well with the experimental data at En= 14.1 MeV and the deviation from calculated results and     

Pre-formation Probability of ^5He Cluster in Pre-equilibrium Mechanism

A new reaction model for light nuclei of lp shell is expanded to ^19F with 2s-ld shell nucleus. The double-differential cross sections of total outgoing neutron for n＋^19F reactions at En = 14.2 MeV are calculated and analyzed, and the calculated results agree fairly well with the experimental measurements.     

Cross Section Measurement in Neutron Energy Range of 6～12 MeV

Introduction The cross section measurements in neutron energy range from 6 to 12 MeV for the reactions with low threshold are very important to obtain a whole excitation function and to make datum eveluation. But in this energy range, purely monoenergitic neutron source is not available, which make the measured data very few. And there is a serious effect of low energy neutrons on the activation cross section measurement. The correction for the effect of the low energy neutrons are not sufficient for some available data, which cause the published data largely discrepant.     

Theoretical Study of ~2H(d,γ)~4He Reaction Below E_(cm)<3 MeV

The reaction cross sections of 2H(d,γ)4He at the astrophysically interesting energies (about below few hundreds of keV) are extremely low. Presently it is impractical to measure in the laboratory. Therefore the theoretical investigation is required to pr…     

Magnetic Moment Measurement of ^28p

The last proton separation energy of β-emitting nuclide ^28p is 0.6 MeV and its last proton occupies the orbit 2s1/2. At present, all of the results showed that there exists proton halo structure in ^28p, whether from the measurements of cross section or from the theoretical study. No magnetic moment or quadrupole moment of ^28p have been reported until now. But the value of nuclear moments is a very important experimental data for the decision of halo structure.     

Optimal Reactions for Synthesis of Superheavy Nucleus ^270Hs

The macroscopic-microscopic approach predicts a strong proton-deformed shell at Z=108 to be a partner for the neutron shell at N=162. Thus the nucleus ^270Hs is expected to be a relatively strongly bound ＂double-magic＂ deformed nucleus. Therefore, it is of great interest to synthesize the nucleus 27~Hs and to investigate its structure experimentally. However,