Rn-Th偶偶核的八级形变研究

用推转壳模型在多维形变空间系统研究了Rn-Th偶偶核的基态性质及高自旋情形下的性质, 其中选取的形变自由度为β₂, β₃, β₄和β₅. 计算结果很好的再现了实验提取的转动惯量值. 势能面的研究表明, 随中子数的增加, 基态形状由近球形(N≈130)逐渐演变为八极形变(N≈136)后又发展成为稳定的四极形变(N≥140). 推转计算表明Rn-Th偶偶核的八极形变非常软, 在推转到高自旋情形下, 逐渐变为反射对称形变.     

原子核形变与价核子数的系统关系

利用N_pN_n方法研究了A≥100的偶–偶核基态四极形变参数β的系统规律.根据质量数以及价质子(中子)是粒子还是空穴对原子核分组,发现β与(N_pN_n)^1/2的关系曲线是平滑的.不同组中原子核的β变化曲线的斜率和趋势显示,价核子和空穴对核四极形变的贡献不同.通过对近滴线原子核理论形变值的变化规律的研究表明,在N_pN_n方法中p-n价核子相互作用的一般关系可能依然适用于不稳定核.     

稀土区奇A核晕带存在从转动到振动形状演化的直接证据(英文)

原子核的形状演化效应是核结构研究的重要基础问题之一。通常认为,A=160质量区的奇A核位于大形变核区域,它们的激发态能谱将呈现出典型的转动激发特征。然而,基于E-GOS曲线方法,发现随着角动量的增加,该质量区奇A核的晕带具有显著地从转动激发演化成为振动激发的形状演化现象。此外,为深入理解原子核形状演化的微观机制,采用Total-Routhian-Surface（TRS）方法针对稀土区的奇A核进行了理论计算,结果表明,165Yb和157Dy同位素在低激发态时具有稳定的长椭形变,当角动量大于0.50 MeV后,核芯的四极形变显著减小并开始产生三轴形变。The phase transition of nuclei with increasing angular momentum (or spin) and excitation energy is one of the most fundamental topics of nuclear structure research. The odd-N nuclei with A ≈160 are widely considered belonging to the well-deformed region, and their excitation spectra are energetically favored to exhibit the rotational characteristics. In this work, however, the evidence suggesting that the nuclei changes from rotation to vibration along the yrast lines as a function of spin was found. The simple method, named as E-Gamma Over Spin (E-GOS) curves, would be used to discern the evolution from rotational to vibrational structure in nuclei for various spin ranges. Meanwhile, in order to understand the band structure properties of nuclei, theoretical calculations have been performed for the yrast bands of the odd-A rare-earth nuclei within the framework of the total routhian surface (TRS) model. The TRS plots predict that the 165Yb and 157Dy isotopes have large quadrupole shapes at low spin states. At higher rotational frequency (hω~ >0.50 MeV), a clear reduction of the quadrupole deformation is indicated by the present results, and the isotopes become rigid in the γ deformation.     

Alignments in the nobelium isotopes

Total-Routhian-Surface calculations have been performed to investigate the deformation and alignment properties of the No isotopes. It is found that normal deformed and superdeformed states in these nuclei can coexist at low excitation energies. In neutron-deficient No isotopes, the superdeformed shapes can even     

Spin-orbit potential in sulfur isotopes

The effects of the spin-orbit interaction in exotic nuclei are investigated by studying the binding energies and deformations of Si, S and Ar isotopes. The calculations were obtained by Skyrme-Hartree-Fock model with various spin-orbit potentials. The results reveal that spin-orbit potential is important in neutron rich nuclei.     

76Se三声子态成员的候选者

通过⁷⁶Br (T_1/2=16.2h)β⁺/EC衰变方法得到⁷⁶Br衰变纲图, 并确认了Muller等通过核反应⁷⁶Se(p, p′)方法发现⁷⁶Se能级纲图中1791.31keV能级. 不过, Muller等当时并没有指出该条能级的自旋和宇称, 以及应该属于哪一个声子态的成员. 经过分析我们认为1791.31keV能级可以作为⁷⁶Se三声子态的一个候选成员. 此外, 为了研究这个介于强形变和球形核之间的过渡区核的形变, 对它的正宇称态进行了采用推转壳模型形式的总转动能面计算.     

奇A核Pd同位素中h_(11/2)入侵轨道的形状驱动效应研究

过渡区原子核的形变与准粒子占据的轨道密切相关。采用推转壳模型首次系统性地研究了奇A核~(99)Pd,~(101)Pd和~(103)Pd原子核中h_(11/2)轨道对核芯的形状驱动效应,基于Total-Routhian-Surface(TRS)方法的计算结果表明,当过渡区原子核~(99)Pd,~(101)Pd和~(103)Pd中的准粒子开始占据h_(11/2)入侵轨道时将会使原子核产生稳定的四极形变。另外,对A≈210质量区近滴线核的高自旋态研究现状及今后进一步的工作也进行了概述。     

169Re的转动带结构组态相关性研究

研究了¹⁶⁹Re的高自旋态能级结构,建立了组态为π9/2^－[514]的强耦合带和组态为π1/2^－[541]的退耦合带,推转壳模型(Cranked shell model)计算结果表明组态相关的不同形变能够解释这些转动带的不同带交叉频率,在已知的奇ARe核中,¹⁶⁹Re的9/2^－[514]转动带在低自旋时具有最大的能量旋称劈裂,当一对i_13/2中子顺排后,旋称劈裂发生了反转,并且劈裂的幅度非常显著地减少了,另外,还观测到了一个三准粒子激发带,并指定了它的最可能组态为π9/2^－[514]⊙νAE。     

核科学百年讲座第一讲 历史性发现及其对人类社会的影响(Ⅰ)

第一讲和第二讲系统地介绍了核科学发展历史，特别是核科学中的历史性发现和重大应用．主要综述核科学的早期发展历史，总体介绍核科学中最基本的重大发现，如放射性、电子、质子、中子、原子核裂变和衰变的发现．介绍人类认识原子和原子核的历史过程，包括与之相关的著名实验和理论．通过介绍核科学的发展和应用，展示了核科学技术对自然科学本身及其对人类社会的深远影响和巨大贡献．     

前中子星内的K-凝聚和超子的生成

用相对论平均场下的手征强子模型研究了前中子星内K^-凝聚和超子的生成。结果显示，前中子星内的中微子束缚使得出现K^-凝聚的临界密度推迟到更高的重子密度，而K^-0凝聚无法出现。同时中微子束缚使得前中子星的状态方程变硬，从而前中子星的最大质量变大。如果考虑超子，前中子星内无法出现K^-凝聚，同时系统的状态方程变软（与不含超子的情况相比），从而对应前中子星的最大质量变小。A chiral hadronic model is extended to investigate antikaon condensation and hyperons production of protoneutron stars. Our results show that neutrino trapping makes the critical density of K^- condensation delay to higher density and K^-0 condensation not occur. Meanwhile, the equation of state （EOS） of （proto）neutron star matter considering neutrino trapping is stiffer than the case without neutrino trapping. Therefore the maximum masses of rotoneutron stars with neutrino trapping are larger than those without neutrino trapping. If hyperons are considered, antikaon condensation does not appear in （proto） neutron stars. Meanwhile, the corresponding EOS becomes much softer, and the maximum masses of （proto）neutron stars are smaller than those without hyprons.