Determination of Astrophysical 13N（p,γ）^14O S-factors from the Asymptotic Normalization Coefficient of ^14C→^13C ＋ n

The angular distribution of the ^13C（d,p）^14C reaction is reanalysed using the Johnson-Soper approach. The squared asymptotic normalization coefficient （ANC） of virtual decay ^14 C →^13 C^14＋ n is then derived to be 21.4±5.0 fm^-1. The squared ANC and spectroscopic factor （SF） of ^14O→^13N ＋p are extracted to be 30.4± 7.1 fm^-1 and 1.94 ± 0.45, respectively. The astrophysical S-factors and reaction rates of ^13N（p, γ）140 are determined from the ANC of ^14O → ^13N ＋ P using the R-matrix approach.     

Test of Determination of (p,γ) Astrophysical S-Factors Using the Asymptotic Normalization Coefficients from Neutron Transfer Reactions

The asymptotic normalization coefficients （ANCs） for the virtual decay ^17 O→^16 O＋n are derived from the angular distributions of the 16 O（d, p）^17O reaction leading to the ground and first excited states of ^17O, respectively, using the distorted wave Born approximation and the adiabatic wave approximation. The ANCs of ^17F are then extracted according to charge symmetry of mirror nuclei and used to calculate the astrophysical S-factors of ^16 O（p, γ）^17 F leading to the first two states of ^17 F. The present results are in good agreement with those from the direct measurement. This provides a test of this indirect method to determine direct astrophysical S-factors of （P, γ） reaction. In addition, the S-factors at zero energy for the direct captures to the ground and first excited states of ^17 F are presented, without the uncertainty associated with the extrapolation from higher energies in direct measurement.     

Resonance states in 16O+16O, 12C+16O, α+16O and α+12C with modified Morse potentials

The resonance states in ¹⁶O+¹⁶O, ¹²C+¹⁶O, α+¹⁶O and α+¹²C are described using modified Morse potential proposed earlier whose success has already been demonstrated in the case of ¹²C+¹²C system. The general validity of such a potential with long range, shallow depth and repulsive soft core determined from the resonance data itself is being examined through the present study of the resonances in the above four systems. In each system, the experimental data of a large number of states have been successfully described with a modified Morse potential. The success points out a common mechanism of the origin of these states, and reaffirms authentically the diatomic-like rotational and vibrational picture of the nuclear molecular resonances proposed previously. The close resemblance between the physics of diatomic molecules and nuclear molecular resonances extending to the level of potential which is Morse type in both the cases — although belong to two different areas of physics — is further strengthened through the present study.      

在独立α集团模型下对敲出反应16O(p,pα)12C和16 O(α,2α)12C的研究

在独立α集团模型下，利用扭曲波冲量近似(DWIA)，计算了实验室系下入射能量为101.5MeV 的敲出反应¹⁶O(p，pα)¹²C和实验室系下入射能量分别为90Me V和140MeV 的敲出反应¹⁶O(α,2α)¹²C.得到的反应截面和谱因子与实 验数据基本符 合，比用壳模型的结果有了一定的改进，表明独立α集团模型能较好地描述α集团敲出反应 的机理. 关键词： α集团模型 敲出反应 反应截面 谱因子     

Astrophysical S-factor of the d(p,γ)3He processby

We summarize the recent effective field theory (EFT) studies of low-energy electroweak reactions of astrophysical interest, relevant to big-bang nucleosynthesis. The zero energy astrophysical S(0) factor for the thermal proton radiative capture by deuteron is calculated with pionless EFT. The astrophysical S(0) factor is accurately determined to be S(0)=0.243 eV·b up to the leading order (LO). At zero energies, magnetic transition M₁ gives the dominant contribution. The M₁ amplitude is calculated up to the LO. A good, quantitative agreement between theoretical and experimental results is found for all observables. The demonstrations of cutoff independent calculation have also been presented.     

Determination of nuclear vertex constants (asymptotic normalization coefficients) for the virtual decays 3He → d + p and 17F → 16O + p and their use for extrapolating astrophysical S -factors of the radiative proton capture by the deuteron and the 16O nucleus at very low energies

Experimental astrophysicalS-factors for the direct radiative capture processes d(p,γ)³He and ¹⁶O(p,γ)¹⁷F are analyzed using the modified two-body potential approach. The values of the asymptotic normalization coefficients (nuclear vertex constants) are found for the wave functions of the ³He and ¹⁷F nuclei in the (d + p) and (¹⁶O + p) channels respectively and are then used to extrapolate the astrophysical S-factor to the region of very low energies. Original Russian Text ? S.V. Artemov, S.B. Igamov, K.I. Tursunmakhatov, R. Yarmukhamedov, 2009, published in Izvestiya Rossiiskoi Akademii Nauk. Seriya Fizicheskaya, 2009, Vol. 73, No. 2, pp. 176–181.     

Astrophysical S-factor of the d(p,γ)3He processby

We summarize the recent effective field theory (EFT) studies of low-energy electroweak reactions of astrophysical interest, relevant to big-bang nucleosynthesis. The zero energy astrophysical S(0) factor for the thermal proton radiative capture by deuteron is calculated with pionless EFT. The astrophysical S(0) factor is accurately determined to be S(0)=0.243 eV·b up to the leading order (LO). At zero energies, magnetic transition M₁ gives the dominant contribution. The M₁ amplitude is calculated up to the LO. A good, quantitative agreement between theoretical and experimental results is found for all observables. The demonstrations of cutoff independent calculation have also been presented.     

12C(7Li,t)16O和20Ne(d,6Li)16O反应的研究

本文把用于处理重离子引起的单粒子转移反应的Goldfarb-Buttle方法推广到多粒子转移反应。计算了¹²C(⁷Li,t)¹⁶O和²⁰Ne(d,⁶Li)¹⁶O反应,用了¹⁶O的全相干波函数,考虑了某些反冲因素,并将结果与实验作了比较。     

Estimation of radiative capture 13B(n,γ0+1)14B reaction rate in the modified potential cluster model

We discuss current attempts to employ the modified potential cluster model to describe the available experimental data on the ¹³B(n,γ₀₊₁)¹⁴B total cross-sections.The estimated results of the M1 and E1 transitions from the n¹³B scattering states to the ground and first excited states of ¹⁴B are presented.The 1^st resonance at E_x=1.275MeV(1⁺) is revealed in both the cross-section and reaction rate.Within the var...     

12C+209Bi和14N+Pb裂变反应碎片角分布和激发函数测量

本工作采用固体核径迹探测器(天然白云母)和金硅面垒型半导体探测器测量了¹²C+²⁰⁹Bi和¹⁴N+Pb裂变反应的碎片角分布和激发函数.由碎片角分布各向异性提取的鞍点有效转动惯量J₀/J_eff与转动有限力程模型(RFRM)做了比较.用统计蒸发模型计算的裂变激发函数拟合实验数据,研究了裂变位垒的角动量效应.     

58Ni(n,p),60Ni(n,p),62Ni(n,α)和54Fe(n,p)反应截面的测量与评价

本实验用活化法测量了中子能量在13.60MeV—17.77MeV的⁵⁸Ni(n,p)^58m+gCo,⁶⁰Ni(n,p)⁶⁰Co和⁶²Ni(n,α)⁵⁹Fe三个反应道的反应截面值,并计算了反应截面测量误差的协方差矩阵.实验的测量误差在3%—7%范围内.     

100Mo(n2n)99Mo,96Mo(n,p)96Nb和92Mo(n,α)89m+gZr反应截面测量

本文报告了在E_n=13.40—14.79MeV中子能区用活化法以²⁷Al(n,α)²⁴Na截面为中子注量标准测行的¹⁰⁰Mo(n2n)⁹⁹Mo,⁹⁶Mo(n,p)⁹⁶Nb和⁹²Mo(n,α)^89m+gZr的反应截面,中子能量是用铌锆截面比法测定的.文中将实验测量值与理论计算值进行了比较,还对上述三个反应的截面进行了编评,给出了推荐的激发曲线.     

59Co(n,p)59Fe,59Co(n,α)56Mn,59Co(n,2n)58Co反应截面的测量

本实验用活化法测量了中子能量在12.8MeV到17.8MeV的⁵⁹Co(n,p)⁵⁹Fe,⁵⁹Co(n,α)⁵⁶Mn,⁵⁹Co(n,2n)⁵⁸Co三个反应道的反应截面值,实验的测量误差在3.3%—6.9%范围内.     

Comparison of asymptotic normalization coefficients for 10B → 9B + n and 10B → 9Be + p configurations obtained from 10B(d,t)9B and 10B(d,3He)9Be reactions

The differential cross sections of the ¹⁰B(d,t)⁹B and ¹⁰B(d,³He)⁹Be reactions at E _d = 25 MeV were measured to obtain the ratio of asymptotic normalization coefficients for the bound states of the last neutron and the last proton in the symmetric nucleus ¹⁰B. The obtained ratio is shown to be in agreement with the theoretical value.     

Signals of α clusters in 16O+16O collisions at the LHC from relativistic hydrodynamic simulations

In relativistic heavy ion collisions, the fluctuations of initial entropy density convert to the correlations of final state hadrons in momentum space through the collective expansion of strongly interacting QCD matter. Using a (3+1)D viscous hydrodynamic program, CLVisc, we consider whether the nuclear structure, which provides initial state fluctuations as well as correlations, can affect the final state of heavy ion collisions, and whether one can find signals of α cluster structures in oxygen using final state observables in \begin{document}$ ^{16}\text{O}+{}^{16}\text{O} $\end{document} collisions at the CERN Large Hadron Collider. For the initial nucleon distributions in oxygen nuclei, we compare three different configurations, a tetrahedral structure with four-α clusters, the deformed Woods-Saxon distribution, and a spherical symmetric Woods-Saxon distribution. Our results show that the charged multiplicity as a function of centrality and the elliptic flow at the most central collisions using the four-α structure differs from those with the Woods-Saxon and deformed Woods-Saxon distributions, which may help to identify α clustering structures in oxygen nuclei.     

Spin structure of the “forward” charge-exchange reaction n + p → p + n and deuteron charge-exchange breakup d + p → (pp) + n

The spin structure of the nucleon charge-exchange process n + p → p + n is investigated. Analysis shows that the spin-dependent part of the differential cross section of the process n + p → p + n at zero angle, which is proportional to the differential cross section of the deuteron charge-exchange breakup d + p → (pp) + n in the “forward” direction, plays the predominant role in the wide range of neutron momenta.     

Investigation of the near-threshold (γ, n) reaction on the 116Cd and 121Sb nuclei

Isomeric yield ratios of ^115m,g Cd and ^120m,g Sb were measured in the (γ, n) reaction in the near-threshold region at γ-ray energies of 9.6, 9.8, 10.0, and 10.5 MeV. Experimental values of the isomeric yield ratios were compared with theoretical values calculated using the TALYS-1.0 program package. The (γ, n) reaction is shown to have a statistical character in the excitation region of residual nuclei 0.3–1.5 MeV.     

Astrophysical ~(22)Mg(p,γ)~(23)Al reaction rates from asymptotic normalization coefficient of ~(23)Ne→~(22)Ne+n

The radionuclide ~(22)Na generates the emission of a characteristic 1.275 MeV γ-ray. This is a potential astronomical observable, whose occurrence is suspected in classical novae. The ~(22)Mg(p, γ)~(23)Al reaction is relevant to the nucleosynthesis of ~(22)Na in Ne-rich novae. In this study, employing the adiabatic distorted wave approximation and continuum discretized coupled channel methods, the squared neutron asymptotic normalization coefficients(ANCs)231 for the virtual decay of Ne → ~(22)Ne + n were extracted, and determined as(0.483 ± 0.060) fm~(-1) and(9.7 ± 2.3) fm~(-1) for the ground state and the first excited state from the experimental angular distributions of ~(22)Ne(d, p)~(23)Ne populating the ground state and the first excited state of ~(23)Ne, respectively. Then, the squared proton ANC of ~(23)Al_(g.s.) was obtained as C_(d5/2)~(2)(~(23)Al)(2.65 ± 0.33) × 10~3 fm~(-1) according to the charge symmetry of the strong interaction. The astrophysical S-factors and reaction rates for the direct capture contribution in ~(22)Mg(p, γ)~(23)Al were also presented. Furthermore, the proton width of the first excited state of ~(23)Al was derived to be(57 ± 14) eV from the neutron ANC of its mirror state in ~(23)Ne and used to compute the contribution from the first resonance of ~(23)Al. This result demonstrates that the direct capture dominates the ~(22)Mg(p, γ)~(23)Al reaction at most temperatures of astrophysical relevance for 0.33 T_9 0.64.