Nuclear weak interaction rates during stellar evolution and collapse

Nuclear weak interaction rates, including electron and positron emission rates, and continuum electron and positron capture rates , as well as the associated v and –/v energy loss rates are calculated on a detailed grid of temperature and density for the free nucleons and 226 nuclei with masses between A = 21 and 60. Gamow-Teller and Fermi discrete-state transition matrix element systematics and the Gamow-Teller T^< →/← T^> resonance transitions are discussed in depth and are implemented in the stellar rate calculations. Results of the calculations are presented on an abbreviated grid of temperature and density and comparison is made to terrestrial weak transition rates where possible. Neutron shell blocking of allowed electron capture on heavy nuclei during stellar core collapse is discussed along with several unblocking mechanisms operative at high temperature and density. The results of one-zone collapse calculations are presented which suggest that the effect of neutron shell blocking is to produce a larger core lepton fraction at neutrino trapping which leads to a larger inner-core mass and hence a stronger post-bounce shock.

The relative abundances of Sn, Te, Xe, Ba, and Ce in the cosmic radiation

Elements with even atomic number (Z) in the interval 50 ≤ Z ≤ 58 have been resolved in the cosmic radiation using the Heavy Nuclei Experiment on the HEAO-3 satellite. Their relative abundances have been compared with the results expected from pure r-process material, pure s-process material, and solar system material, both with and without a modification due to possible first ionization potential effects. Such effects may be the result of the preferential acceleration, and hence enhancement in the cosmic rays, or those elements having low first ionization potentials. We find that our measurements are inconsistent with pure r-process material at the greater than 98% confidence level whether or not the first ionization potential adjustments are made.

In addition, we have compared our results with mixtures having varying ratios of pure r-process material to pure s-process material. We find that, if no first ionization potential effects are included,

(r/s)CRS/(r/s)SS = 0.20^+0.18_-0.14

where CRS refers to the cosmic ray source and SS refers to the solar system, consistent with having an almost pure s-process source. If the first ionization potential adjustments are applied

(r/s)CRS/(r/s)SS = 1.5^+1.1_-0.7

consistent with a solar system mixture.

The abundances of ultraheavy elements in the cosmic radiation

Analysis of the data from the Heavy Nuclei Experiment on the HEAO-3 spacecraft has yielded the cosmic ray abundances of odd-even element pairs with atomic number, Z, in the range 33 ≤ Z ≤60, and the abundances of broad element groups in the range 62 ≤ Z ≤83, relative to iron. These data show that the cosmic ray source composition in this charge range is quite similar to that of the solar system provided an allowance is made for a source fractionation based on first ionization potential. The observations are inconsistent with a source composition which is dominated by either r-process or s-process material, whether or not an allowance is made for first ionization potential. Although the observations do not exclude a source containing the same mixture of r- and s-process material as in the solar system. the data are best fit by a source having an r- to s-process ratio of 1.22^(+0.25)_(0.21), relative to the solar system The abundances of secondary elements are consistent with the leaky box model of galactic propagation, implying a pathlength distribution similar to that which explains the abundances of nuclei with Z<29.

The energy spectra of the even elements in the range 38 ≤ Z ≤ 60 are found to have a deficiency of particles in the range ~1.5 to 3 GeV/amu, compared to iron. This deficiency may result from ionization energy loss in the interstellar medium, and is not predicted by propagation models which ignore such losses. ln addition, the energy spectra of secondary elements are found to be different to those of the primary elements. Such effects are consistent with observations of lighter nuclei, and are in qualitative agreement with galactic propagation models using a rigidity dependent escape length. The energy spectra of secondaries arising from the platinum group are found to be much steeper than those of lower Z. This effect may result from energy dependent fragmentation cross sections.

Simulation of the Lanzhou Penning Trap LPT

The LPT (Lanzhou Penning Trap) is under construction and its task is to perforin direct mass measurement of fusion-evaporation residue, and if possible for heavy isotopes. Detailed simulations have been clone for a good understanding to the ion's movement and mechanics in the trap. The optimizal ion of the LPT is also performed based on the simulation. With a scale of 0.5 mm per grid used in the, simulation and many other limitations a highest mass resolution has been achieved to be 1.9 x 10(-5). An unexpected behavioin in the simulation related to magnetron motion has been found.

High precision mass measurement and LPT

A Penning trap, which can measure the atomic masses with the highest precision, is one of the most important facilities in nuclear physics research nowadays. The precision mass data play an important role in the studies of nuclear models, mass formulas, nuclear synthesis processes in the nuclear astrophysics, symmetries of the weak interaction and the conserved vector current (CVC) hypothesis. The status of high precision mass measurement around the world, the basic principle of Penning trap and the basic information about the LPT (Lanzhou Penning Trap) are introduced.

Latest progress of the RFQ cooler and buncher RFQ1L

The RFQ cooler and buncher RFQ1L is a key device of the SHANS (Spectrometer for Heavy Atoms and Nucleax Structure). The status of the machining and assembly of the central part is introduced, and the structure of the whole RFQ1L system and the preliminary plan for the testing are discussed also.

Shell correction and pairing energies in the dinuclear system model

We investigate the dependences of the potential energy surfaces (PES) and the fusion probabilities for some cold fusion reactions leading to super-heavy elements on the nuclear shell effect and pairing energy. It is found that the shell effect plays an important role in the fusion of the super-heavy element while pairing energy's contribution is insignificant. The fusion probabilities and evaporation residue cross sections as functions of the Ge-isotope projectile bombarding Pb-208 are also investigated. It is found that evaporation residue cross sections do not always increase with the increasing neutron number of Ge-isotope

Experimental study of the high-voltage breakdown and simulations for the RFQ cooler and buncher RFQ1L

The RFQ cooler and buncher RFQ1L is one of the key parts of the being-built super-heavy nuclide research spectrometer. In order to understand the high-voltage breakdown phenomenon, the voltages between electrodes have been measured. In addition, more extensive simulations have been performed for better understanding and optimizing the RFQ1L work points.

Microscopic examination of NpNn dominance in the evolution of nuclear structure

The proton-neutron interaction in determining the evolution of nuclear structure has been studied by using the Brillouin-Wigner perturbation expansion. The particle-hole and particle-particle p-n interactions are unifiedly described in the theory. The obtained formulas of level energies and excitation energies scaled in the small- and large-NpNn limits can well explain the linearity of the extracted proton-neutron interaction energies and the attenuation of the 2(1)(+) excitation energies against the valence nucleon product NpNn for five mass regions from A = 100-200.

Relativistic Continuum Random Phase Approximation and Applications II. Applications

The fully consistent relativistic continuum random phase approximation (RCRPA) has been constructed in the momentum representation in the first part of this paper. In this part we describe the numerical details for solving the Bethe-Salpeter equation. The numerical results are checked by the inverse energy weighted sum rules in the isoscalar giant monopole resonance, which are obtained from the constraint relativistic mean field theory and also calculated with the integration of the RCRPA strengths. Good agreement between the misachieved. We study the effects of the self-consistency violation, particularly the currents and Coulomb interaction to various collective multipole excitations. Using the fully consistent RCRPA method, we investigate the properties of isoscalar and isovector collective multipole excitations for some stable and exotic from light to heavy nuclei. The properties of the resonances, such as the centroid energies and strength distributions are compared with the experimental data as well as with results calculated in other models.

超重谱仪中冷却聚束器RFQ1L的模拟研究

对超重核和超重元素越来越多的探索和研究，以及对远离β稳定线奇异核的精细研究，都迫切地需要低能量、高品质的放射性束流。然而，由原子核反应产生的放射性束流普遍具有能量分散大、发射度大以及束流斑点大的缺点，因此，对放射性次级束流进行进一步的操控成为深入研究的必需条件。充有缓冲气体的RFQ冷却聚束器是适合这项任务的最佳选择。它不但可以高速度、高效率地提高束流的品质，而且适用于所有的核素。这项技术在上世纪末蓬勃地发展起来，现在已经成为世界各主要实验室进行放射性次级束流操控的必备实验装置。在中国科学院近代物理研究所，一台正在研制的专用于研究长寿命核素的超重核研究谱仪中就使用了RFQ冷却聚束器来冷却、约束和储存离子。论文首先简单介绍了近代物理研究所超重谱仪的情况和国际上RFQ冷却聚束器的研究情况，其次阐述了RFQ冷却聚束器相关原理，然后重点论述了用SIMION程序进行模拟的方法和对RFQ1L冷却段的模拟情况，并对模拟结果进行了讨论，接着，讨论了计算机无法模拟的一些因素，重点讨论了气体击穿问题，最后，对本论文的工作进行了总结，并对下一步工作进行了展望望。对RFQ1L冷却段的模拟和气体击穿问题是本论文的两个重点。冷却段的模拟是以为例进行的。通过改变缓冲气体压强、入射离子能量以及轴向电场梯度，得到了离子在RFQ冷却聚束器中不同的运动情况，得到了一些有意义的结论，有助于设备的设计和工作点的选择。另外，RFQ冷却聚束器的工作区域，正好位于缓冲气体最容易被击穿的范围，再加上射频的影响，因此气体击穿问题成为制约工作点选择的一个非常重要的因素。本文对此也作了详细的讨论

重核性质的相对论平均场理论研究

本论文主要包括两部分内容，一部分是运用相对论平均场理论对超重核基态性质的研究以及Pb同位素位移微观机制的研究，第二部分是在相对论平均场框架下对BCS型对关联的改进及其在有限核性质研究中的应用。基于核子与介子自由度的量子强子动力学(QHD)， 从有效拉氏密度出发, 采取平均场近似, 已经成为当前最为成功的原子核理论之一，相对论平均理论。本文比较详细地介绍该理论模型, 并系统地探讨了新核素287115及其 衰变链上核的基态性质。结果发现所计算的结合能和四极形变符合了有限力程小液滴模型的结果，计算表明研究的 衰变链具有中等大小的长椭球形变；且计算的 衰变能 成功地与实验符合，说明相对平均场理论在原子核的超重区是有成功的。在此基础上进一步研究了新核素的单粒子能级，从而发现了超重核的一些新特点。通过分析Z=108到Z=114这四条同位素链的平均结合能，说明在这些同位素链中，对中子分离能的分析则可以看到N=162与N=184是壳效应的存在。研究了Pb同位素链的基态性质，从原子核的微观结构出发，比较详细地研究了Pb链同位素位移出现反常扭折这一重要性质的物理机制，由于满壳外额外中子会排布在距离满壳稍远一些的下一能级上，这自然会导致中子半径的增加．由于中子在核内的分布对质子分布的影响，将必然使原子核的电荷半径会在中子满壳后增加得更快。相对论平均场理论能够自然地给出原子核的自旋和轨道耦合，从而能给出合理的单粒子能级序列和间距，这为定量描述原子核的同位素位移提供了有力的理论基础。在论文的第二部分，通过引进密度相关的Delta力来改进传统的处理对关联的BCS方法，假定核子之间的作用为Delta力，计算得到状态相关的对能隙。相对于传统的常数对能隙是一个很重要的改进。接着我们用改进的理论研究了Sr同位素链的基态性质，得到了一些很有意义的结果。

基于RIBLL束线开展超重核合成的可行性研究

超重元素合成研究是当今国际上核物理研究的热点领域之一，也是中国科学院近代物理研究所的一个重要研究方向。根据实际情况，我们确定了两步走的发展方案。针对第一步发展方案，我们对RIBLL放射性束流线进行了改造。具体做法就是在RIBLL入口的前段增加一个速度选择器，并将原束流传输线的前半段改造为充气谱仪。本论文详细论述了RIBLL改造所涉及到的硬件设计和建造以及改造后系统的各项性能测试。硬件部分主要包括反应靶室、转靶系统、速度选择器、充气及气压控制系统、焦平面的衰变探测器等。性能测试方面主要开展了以下工作：(1) 利用放射源对速度选择器的接收立体角和动量接收度进行了测试；(2) 测量了铀离子经不同厚度碳膜后的电荷态分布，并与经验公式计算进行了比较；(3) 利用已知截面的反应道和靶反冲核分别对系统的传输效率、充气谱仪的最佳气压值和重离子在氦气中的平衡电荷态进行了研究。基于以上测试的结果，论文对在改造后的RIBLL上开展超重核合成研究的可行性进行了讨论。结论是由于RIBLL的二极磁铁的分析能力太强，大大降低了系统的传输效率，因此该谱仪只可用于原子序数Z≤107的超重核合成研究和生成截面较高的短寿命滴线核的合成及性质研究，对于更高原子序数的超重核合成研究应该放到正在建造的SHANS谱议上进行

Nuclear pairing: surface or bulk?

We analyze how the spatial localization properties of pairing correlations are changing in a major neutron shell of heavy nuclei. It is shown that the radial distribution of the pairing density depends strongly on whether the chemical potential is close to a low or a high angular momentum level and has little sensitivity to whether the pairing force acts at the surface or in the bulk. The pairing density averaged over one major shell is, however, rather flat, exhibiting little dependence on the pairing force. Hartree-Fock-Bogoliubov calculations for the isotopic chain 100-132Sn are presented for demonstration purposes.