太阳系的元素丰度分布与AGB星慢中子俘获元素

通过对AGB星演化模型的理论计算结果和51颗AGB星的观测丰度进行重新分析,发现任何AGB星与慢中子俘获过程(s过程)主要分量对应的重元素(简称SMH元素)丰度分布都与对应的太阳系s过程主要分量的元素丰度分布相似,这表明,任意AGB星SMH元素丰度分布的迭加结果与对应的太阳系s过程主要分量的元素丰度分布相似,由此得出结论:太阳系s过程主要分量的重元素丰度分布模式是一个典型的模式,可以作为标准用于单星重元素丰度的研究.     

间接测量中重放射性核中子俘获截面——替代比率法

s过程中的放射性核素中子俘获截面对天体核合成和核素丰度有重大影响, 在直接测量异常困难的情况下, 替代比率法是获得放射性核素中子俘获截面数据的一种间接新方法。 简单介绍了替代比率法理论, 并简要论述了用替代比率法推导中重核区放射性核素中子俘获截面的可行性。 The radioactive nuclei neutron capture cross section is very important to nuclearsynthesis and nuclide abundance in s process, but it is difficult to be measured directly because of the target production. A new method, surrogate ratio method which is developed from surrogate method, could be used to determine the cross section of radioactive nuclei neutron capture. In this paper, the surrogate ratio method was introduced and the feasibility was discussed to deduce the desired neutron capture cross sections with surrogate ratio method.     

低能中子的俘获γ射线能谱

给出了计算共振区平均中子俘获r能谱的方案。主要考虑了三种反应机制:统计过程、位阱俘获与复弹性道中的俘获脚。具体计算了3s共振区几个核素⁵¹V,⁵²Cr,⁵⁵Mn的热中子俘获r能谱和r光子多重数。结果表明,包括了复弹性道中的俘获这一过程后,理论与实验的符合得到明显的改善,特别是对能谱的高能端。     

中微子是超新星生成重元素的新途径

 恒星在漫长的一生中通过其内部的核聚变放出能量,普遍认为恒星内部是碳和较重元素的诞生地。以这种方式生成的最重元素是铁和镍,一般认为更重的元素是通过慢中子俘获反应(s-过程)和/或快中子俘获反应(r-过程)生成的。尽管对这些核合成机制已经有了一段时间的了解,但是一些元素的丰度仍有未解之谜。瑞士巴塞尔大学(UniversitatBasel)的卡拉·弗勒利希(Car-laFrhlich)和达姆施塔特市(Darmstadt)德国重离子研究所(Gesellschaftf櫣rSchwerionenforschung,GSI)的加百利·马丁斯-潘内多(GabrielMart姫nez-Pinedo)与同事们提出     

基于(p,γ)-(γ,p)平衡近似的快质子俘获过程模型及其应用

在(p,γ)-(γ,p)平衡近似下,本文建立了简化的快质子俘获(rp)过程模型, 讨论了天体物理条件输入量 (即质子辐照时间、质子数密度及温度) 对rp过程的影响. 结合中国科学院近代物理研究所等时性质谱仪 (IMS) 上的最新实验数据, 本文进而分析了新测的缺中子原子核质量对rp过程的影响; 发现利用新测的⁴¹Ti质量, A=41处的丰度相较之前的计算结果增大了两个数量级, 而计算的相对丰度误差减小了近两个量级. 关键词： 快质子俘获过程 γ)-(γ,p)平衡')" href="#">(p,γ)-(γ,p)平衡 原子核质量 缺中子原子核     

一类生灭过程及其在核天体物理计算中的应用

研究一类生灭过程,利用矩阵分解技巧求出了生灭过程微分方程的解,并将之应用于核天体物理中太阳系慢中子俘获过程重元丰度计算问题研究,计算结果与天文观测值一致.     

原子核质量的高精度测量

原子核的质量直接反映了核内强相互作用、电磁相互作用和弱相互作用的结果.文章简要阐述了原子核质量测量的意义、现状和主要方法,介绍了基于兰州重离子冷却储存环的原子核质量测量实验,比较了首次得到的63Ge, 65As,67Se和71Kr核质量测量值与理论计算结果,探讨了65As质量对天体物理快质子俘获过程的影响,文章最后给出了今后的研究内容.中国科学院近代物理研究所在轻质量丰中子区,系统测量了从Ne到Ca核素的质量,研究了N=20和28幻数随中子数和质子数变化的演化;在丰质子区,精确测量了快质子俘获路径上关键核素的质量,为解释X射线暴等爆发性天体过程提供重要的质量数据;在中重丰中子区,系统地测量丰中子核质量,通过天体网络计算模拟超新星爆发中的快中子俘获过程.     

中重核中子辐射俘获γ射线强度函数研究

假设退激过程中除包含巨偶极共振模式外还存在⁶He,⁶Li,⁶Be,⁷Li和⁷Be等粒子集团激发态的退激过程.本文对这一物理假定作了进一步分析.利用据此建立的包括这些过程在内的γ射线强度函数,计算了在核素⁹³Nb,¹⁸¹Ta和天然元素Ag上入射中子能量在0.01—5MeV能区以及在核素¹⁹⁷Au上入射中子能量在0.01—10MeV能区的中子辐射俘获反应截面和γ能谱,得到了与实验数据较好符合的结果.特别是可以较好地解释γ能谱中5.5MeV之后的反常突起.这表明,上述物理假定适用于中重核中子辐射俘获反应.     

MCNP模拟月表关键性元素γ射线与实测结果比较分析

嫦娥一号携带的γ射线谱仪传回大量能谱数据,对其分析与解谱是一个比较复杂的过程。针对此问题,提出按照月表γ射线来源的物理过程,分为月球表面天然放射元素、中子非弹性散射和中子俘获三部分。用MCNP程序模拟其在GRS中的能谱数据,将模拟结果叠加并与实测谱线对比,结果表明,模拟γ谱线能帮助辨识出实测谱线中的部分关键元素,例如~(40)K、~(214)Bi等。     

A=40—70偶中子核素光子穿透系数的关联现象

本文给出了在共振区光子穿透系数的表示式,这由三部份组成,分别对应复合核统计过程、复合核弹性散射道及非弹性散射道中的辐射退激过程.研究了在中子强度函数3s巨共振区13个偶中子核素的中子辐射俘获截面.中子能量范围为3MeV以下的共振区.结果表明,在同时考虑了统计和非统计过程后,可以解释实验测量的总俘获截面及γ能谱.     

The r-process of stellar nucleosynthesis: Astrophysics and nuclear physics achievements and mysteries

The r-process, or the rapid neutron-capture process, of stellar nucleosynthesis is called for to explain the production of the stable (and some long-lived radioactive) neutron-rich nuclides heavier than iron that are observed in stars of various metallicities, as well as in the solar system.

A very large amount of nuclear information is necessary in order to model the r-process. This concerns the static characteristics of a large variety of light to heavy nuclei between the valley of stability and the vicinity of the neutron-drip line, as well as their beta-decay branches or their reactivity. Fission probabilities of very neutron-rich actinides have also to be known in order to determine the most massive nuclei that have a chance to be involved in the r-process. Even the properties of asymmetric nuclear matter may enter the problem. The enormously challenging experimental and theoretical task imposed by all these requirements is reviewed, and the state-of-the-art development in the field is presented.

Nuclear-physics-based and astrophysics-free r-process models of different levels of sophistication have been constructed over the years. We review their merits and their shortcomings. The ultimate goal of r-process studies is clearly to identify realistic sites for the development of the r-process. Here too, the challenge is enormous, and the solution still eludes us. For long, the core collapse supernova of massive stars has been envisioned as the privileged r-process location. We present a brief summary of the one- or multidimensional spherical or non-spherical explosion simulations available to-date. Their predictions are confronted with the requirements imposed to obtain an r-process. The possibility of r-nuclide synthesis during the decompression of the matter of neutron stars following their merging is also discussed.

Given the uncertainties remaining on the astrophysical r-process site and on the involved nuclear physics, any confrontation between predicted r-process yields and observed abundances is clearly risky. A comparison dealing with observed r-nuclide abundances in very metal-poor stars and in the solar system is attempted on grounds of r-process models based on parametrised astrophysics conditions. The virtues of the r-process product actinides for dating old stars or the solar system are also critically reviewed.     

Challenge on the Astrophysical R-Process Calculation with Nuclear Mass Models

Our understanding of the rapid neutron capture nucleosynthesis process in universe depends on the reliability of nuclear mass predictions. Initiated by the newly developed mass table in the relativistic mean field theory (RMF), we investigate the influence of mass models on the r-process calculations, assuming the same astrophysical conditions. The different model predictions on the so far unreachable nuclei lead to significant deviations in the calculated r-process abundances.     

Nucleosynthesis of heavy elements in the r-process

The current state of the problem of heavy-element production in the astrophysical r-process is surveyed. The nucleosynthesis process in the neutron-star-merger scenario, within which the problem of free-neutron source is solved, is considered most comprehensively. A model that describes well the observed abundances of heavy elements is examined. Theoretical approaches used in this model to calculate a number of features of short-lived neutron-rich nuclei are described. The contributions of various fission processes to the production of heavy elements are assessed. The possibility of superheavy-element production in the r-process is demonstrated.     

Neutron-Capture Elements in the Double-Enhanced Star HE 1305-0007： a New s- and r-Process Paradigm

The star HE 1305-0007 is a metal-poor double-enhanced star with metallicity [Fe/H] = -2.0, which is just at the upper limit of the metallicity for the observed double-enhanced stars. Using a parametric model, we find that almost all s-elements were made in a single neutron exposure. This star should be a member of a post-commonenvelope binary. After the s-process material has experienced only one neutron exposure in the nucleosynthesis region and is dredged-up to its envelope, the AGB evolution is terminated by the onset of common-envelope evolution. Based on the high radial-velocity of HE 1305-0007, we speculate that the star could be a runaway star from a binary system, in which the AIC event has occurred and produced the r-process elements.     

Influence of strong magnetic field on β decay in the crusts of neutron stars

βdecay in the strong magnetic field of the crusts of neutron stars is analysed by an improved method. The reactions ⁶⁷ Ni(β^-)⁶⁷ Cu and ⁶² Mn\beta ^-62 Fe are investigated as examples. The results show that a weak magnetic field has little effect on βdecay but a strong magnetic field (B>10¹²G) increases β decay rates obviously. The conclusion derived may be crucial to the research of late evolution of neutron stars and nucleosynthesis in r-process.     

Long, cold, early r process? Neutrino-induced nucleosynthesis in He shells revisited

We revisit a ν-driven r-process mechanism in the He shell of a core-collapse supernova, finding that it could succeed in early stars of metallicity Z ? 10?3 Z(⊙), at relatively low temperatures and neutron densities, producing A ~ 130 and 195 abundance peaks over ~10-20 s. The mechanism is sensitive to the ν emission model and to ν oscillations. We discuss the implications of an r process that could alter interpretations of abundance data from metal-poor stars, and point out the need for further calculations that include effects of the supernova shock.     

Pro duction of Exotic Nuclei in Low-Energy Multi-Nucleon Transfer Reactions

Multinucleon transfer processes in low-energy heavy ion collisions open a new field of research in nuclear physics, namely, production and studying properties of heavy neutron rich nuclei. This not-yet-explored area of the nuclear map is extremely important for understanding the astrophysical nucleosynthesis and the origin of heavy elements. Beams of very heavy U-like ions are needed to produce new long-living isotopes of transfermium and superheavy elements located very close to the island of stability.The calculated cross sections are high enough to perform the experiments at available accelerators.Beams of medium-mass ions (such as 136Xe, 192Os, 198Pt) can be used for the production of neutron rich nuclei located along the neutron closed shell N = 126 (the last waiting point) having the largest impact on the astrophysical r-process. The Low-energy multinucleon transfer reactions is a very efficient tool also for the production and spectroscopic study of light exotic nuclei. The corresponding cross sections are 2 or 3 orders of magnitude larger as compared with high energy fragmentation reactions.     

Calculation of astrophysical reaction rate of 82Ge(n,γ)83Ge

The neutron capture reaction on a neutron-rich near closed-shell nucleus 82Ge may play an important role in the r-process following the fallout from nuclear statistical equilibrium in core-collapse supernovae.By carrying out a DWBA analysis for the experimental angular distribution of 82Ge(d, p)83Ge reaction we obtain the single particle spectroscopic factors, S2,5/2 and S0,1/2 for the ground and first excited states of 83Ge=82Ge(⊕)n, respectively. And then these spectroscopic factors are used to calculate the direct capture cross sections for the 82Ge(n, γ)83Ge reaction at energies of astrophysical interest. The optical potential for neutron scattering on unstable nucleus 82Ge is not known experimentally. We employed a real folding potential which was calculated by using the proper 82Ge density distribution and an effective nucleon-nucleon force DDM3Y.The neutron capture reactions on neutron-rich closed-shell nuclei are expected to be dominated by the direct capture to bound states. We will show that the direct capture rates on these nuclei are sensitive to the structure of the low-lying states.