Sm~(2+)离子的激发态能级

本文采用U群方法计算了Sm~(2+)离子的激发态4f~5n′l′的主要谱项能级,给出了以Slater积分为参数的表达式。并顾及自旋-轨道耦合,按Russell-Saunders近似计算了相应能级的耦合参数λ。     

用费米子动力对称模型(FDSM)计算~(110～116)Cd,~(122～128)Te能谱

按照费米子动力对称模型,计算了Cd和Te若干同位素(偶偶核)的能谱,所得结果与实验符合得较好。     

Properties of hybrid stars in an extended MIT bag model

The properties of hybrid stars are investigated in the framework of the relativistic mean field theory （RMFT） and an MIT bag model with density-dependent bag constant to describe the hadron phase （HP） and quark phase （QP）, respectively. We find that the density-dependent B（p） decreases with baryon density p; this decrement makes the strange quark matter become more energetically favorable than ever, which makes the threshold densities of the hadron-quark phase transition lower than those of the original bag constant case. In this case, the hyperon degrees of freedom can not be considered. As a result, the equations of state of a star in the mixed phase （MP） become softer whereas those in the QP become stiffer, and the radii of the star obviously decrease. This indicates that the extended MIT bag model is more suitable to describe hybrid stars with small radii.     

包含Δ共振态的核物质

在相对论平均场理论框架下研究了包括Δ共振态核物 质的状态方程. 研究表明, 随着Δ粒子相对数密度的增加, 饱和点处的结合能下降, 并向总粒子数密度增加方向移动, 状态方程逐渐变软. 结果表明, 包括Δ粒子的中子星物质是中子星一个可能的相结构.     

复合粒子表象~(20)O基态波函数

讨论复合粒子表象理论（CPRT）的波函数，并计算20O基态CPRT的波函数，结果表明，其费米子空间部分就是壳模型波函数．由此进一步表明复合粒子表象完全等价于通常的量子力学表象。     

Thermal protoneutron stars with hyperons

The properties of thermal protoneutron star matter including hyperons are investigated in the framework of the relativistic mean field theory (RMFT). In protoneuron star matter, with the increase of the temperature, the critical densities of hyperons decrease, the sequence for appearances of hyperons change, the abundances of hyperons as well as neutrinos increase, and the strong interactions between baryons get weaker. Meanwhile, the abundances of isospin multiple states for nucleons, Σ, and Ξ become identical, leading to isospin saturated symmetric matter, respectively. Moreover, if a protoneutron star is born with higher temperature, it is less likely to convert to a black hole.     

K0 Condensation in Hyperonic Neutron Star Matter

In the framework of the relativistic mean field theory, we investigate K^0 condensation along with K^- condensation in neutron star matter including the baryon octet. The results show that both K^0 and K^- condensations can occur well in the core of the maximum mass stars for relatively shallow optical potentials of K^- in the range of-100 MeV～ -160 MeV. With the increasing optical potential of K^-, the critical densities of K^- decrease and the species of baryons appearing in neutron stars become fewer. The main role of K^0 condensation is to make the abundances of particles become identical leading to isospin saturated symmetric matter including antikaons, nucleons and hyperons. K^- condensation is chiefly responsible for the softening of the corresponding equation of state, which leads to a large reduction in the maximum masses of neutron stars. In the core of massive neutron stars, neutron star matter including rich particle species, such as antikaons, nucleons and hyperons, may exist.     

中子-质子费米子动力对称模型下核素Xe,Ba和Ce的低激发谱

探讨了在实际原子核体系中存在的区分中子-质子的SO（6）动力学对称性，并利用这种动力学对称性对过渡区的偶-偶核Xe，Ba和Ce等同位素的低激发谱进行了研究．所得理论结果与实验数据相符合．     

超子耦合常数对混合星性质的影响

用相对论平均场理论描述强子物质, 用NJL模型描述夸克物质研究了超子耦合常数对混合星性质的影响. 结果表明, 随着超子耦合常数的增大, 强子-夸克相变密度变小, 混合相区域的状态方程变硬, 中子星的最大质量及对应的半径变大. 超子耦合常数由0.73增到1.0时, 混合星最大质量由1.68M_⊙增至1.84M_⊙, 相应的半径由11.4km变到12.5km. 该夸克模型下不同强子参数组对应的混合星性质也有较明显的差异. 可知, 其适合于描述大质量而小夸克核心的混合星.