相对论平均场理论中的有效超子-核子相互作用

利用相对论平均场理论,结合单超核的实验数据,研究了核介质中的Λ超子–核子有效相互作用.通过符合13ΛC超核中Λ超子1s轨道的结合能实验值,给出了5组Λ超子–核子有效相互作用参数.利用这些参数组对质量数从9到2?0?8的单Λ超核和核物质中最低Λ态的束缚能进行了系统计算,得到的结果与实验值相符.     

中子星的相对论平均场研究

在相对论平均框架内计算了不同超子耦合参数下中子星内部物质的状态方程,进一步求解Oppenheimer-Volkoff方程得到了中子星的各种性质.结果表明,参数的变化对这些性质有明显的影响.     

208ΛPb的超子分布半径和中子星结构

从相对论平均场理论出发,考虑核子、超子和介子自由度,研究了208ΛPb的超子分布半径与中子星的性质以及它们之间的关系. 计算发现当超子的耦合常数比值由0.3增大到1时,对NLSH和NL3参数组,超核的超子分布半径分别由3.905和3.849fm增大到4.346和4.230fm,而中子星的最大质量分别由1.516和1.429M⊙增大到2.776和2.744M⊙,质量为1.4M⊙的中子星半径分别由13.13和12.79km增大到13.24和13.29km.即中子星的最大质量和半径随超子分布半径增大而增加. 这样只要从实验上确定208ΛPb的超子分布半径,就可以得到中子星结构的信息.     

超子耦合参数对热前中子星物质的影响

在相对论平均场理论框架内,利用Λ超子的结合能和中子星质量的观测数据得到超子标量介子耦合参数χσ的范围是0.33—0.77。在这个范围内, 研究了χσ取不同值时, 包含核子, Λ和Ξ超子的热前中子星（固定单个重子熵s=1）的性质。结果表明, 如果超子耦合参数变大, 前中子星核心温度变高, 中微子丰度变低, 前中子星的亚稳态质量范围变小。如果χσ超过了0.75, 前中子星不可能演变成黑洞。联系SN1987A讨论了这一结果的意义。In the framework of the relativistic mean field theory(RMFT), protoneutron stars with hyperons are studied. To be compatible with neutron star masses, the hyperon scalar coupling χσ should lie in the range of 0.33—0.77. As the hyperon scalar coupling increases, in protoneutron star matter, the core temperature increases whereas the abundance of neutrinos decreases. The metastable mass range of protoneutron stars narrows as the temperature increases. It is found that a protoneutron star cannot subside into a low mass black hole when χσ>0.75. Furthermore, the case of SN1987A is discussed.     

A^208Pb的超子分布半径和中子星结构

从相对论平均场理论出发，考虑核子、超子和介子自由度，研究了A^208Pb的超子分布半径与中子星的性质以及它们之间的关系。计算发现当超子的耦合常数比值由0．3增大到1时，对NLSH和NL3参数组，超核的超子分布半径分别由3．905和3．849fm增大到4．346和4．230fm，而中子星的最大质量分别由1．516和1．429M增大到2．776和2．744M，质量为1．4M的中子星半径分别由13．13和12．79km增大到13．24和13．29km。即中子星的最大质量和半径随超子分布半径增大而增加。这样只要从实验上确定A^208Pb的超子分布半径，就可以得到中子星结构的信息。     

_Λ~(208)Pb的超子分布半径和中子星结构

从相对论平均场理论出发 ,考虑核子、超子和介子自由度 ,研究了2 0 8ΛPb的超子分布半径与中子星的性质以及它们之间的关系 .计算发现当超子的耦合常数比值由 0 .3增大到 1时 ,对NLSH和NL3参数组 ,超核的超子分布半径分别由3 .90 5和 3 .849fm增大到 4.3 4 6和 4.2 3 0fm ,而中子星的最大质量分别由 1 .51 6和1 .42 9M⊙ 增大到 2 .776和 2 .744M⊙ ,质量为 1 .4M⊙ 的中子星半径分别由 1 3 .1 3和 1 2 .79km增大到 1 3 .2 4和 1 3 .2 9km。即中子星的最大质量和半径随超子分布半径增大而增加 .这样只要从实验上确定2 0 8ΛPb的超子分布半径 ,就可以得到中子星结构的信息     

利用密度相关的相对论平均场理论对核物质与中子星的研究(英文)

研究和详细地比较了RMF理论中不同的有效相互作用强度的密度依赖性, 并且讨论了这种密度依赖性对于核物质和中子星性质的影响. 对于核物质, 不同的参数组给出的对称核物质的饱和点非常接近, 基本都在经验值的范围内. 对于中子星, 考虑超子后不同参数组给出的质量极限的范围为1.52—2.06 M☉, 半径为10.24—11.38 km.The density dependencies of various effective interaction strengths in the relativistic mean field and their influences on the properties of nuclear matter and neutron stars are studied and carefully compared. The differences of saturation properties given by various effective interactions are subtle in symmetric nuclear matter. The Oppenheimer Volkoff mass limits of neutron stars calculated from different equations of state are 1.52—2.06 M☉, and the radii are 10.24—11.38 km with hyperons included.     

单极巨共振的相对论平均场计算

利用最近完成的相对论平均场理论的计算程序,研究了原子核单极巨共振.计算了¹⁶O,⁴⁰Ca和²⁰⁸Pb的同位旋标量和同位旋矢量单极巨共振.得到的结果与实验符合较好.     

相对论平均场理论框架下对能的系统研究

在相对论平均场模型的框架内,沿原子核的稳定线,以每隔4个质子或中子提取样本的方法,计算了核谱图上数十个原子核的对能,特别是研究了氧同位素偶-偶核的对能随核子数的变化规律,发现在固定能隙Δ的条件下,对能的大小和核的壳结构有关,由此提出了一种检验闭壳效应的简便方法,进而发现中子数N=6不仅在轻核的丰中子区是一个新幻数,而且在丰质子区也是一个可能的新幻数. 关键词： 相对论平均场模型 对能 能隙 幻数     

超子中子星性质的温度效应

从相对论平均场理论出发,考虑核子、超子和介子的相互作用,研究了温度对中子星组成粒子、状态方程和中子星质量等的影响.发现温度越高,超子在中子星内部出现时的重子数密度越低.当密度较高时,中子星的核心区主要由超子组成,即中子星转变成以奇异粒子为主要成分的超子星,并且这种转变受到温度的影响,温度越高,转变密度越低.由于超子的出现,中子星核心高密度区域的状态方程,对于不同温度,差别不大,所以有限温度中子星的最大质量都在1.8M_⊙附近.这与观测结果相符.     

A Relativistic Model for Strange Quark Star

We propose a relativistic model for strange quark stars within the framework of MIT Bag model. In our model, we assume that the highly compact strange stars are anisotropic in nature which is an expected feature in the ultra high density regime. We discuss various physical features of the model and show that the model satisfies all the regularity conditions. By estimating the value of the Bag constant for strange star candidates like 4U 1820-30, Her X-1 and SAX J 1808.4-3658, we show that a wire range of values of the Bag constant are possible for such stars though, in the case of 4U 1820-30, the estimated value of the Bag constant has been found to be very close to its currently acceptable range. Nevertheless, our results are in agreement with the recent CERN-SPS and RHIC data.     

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.     

RMF理论对N=60同中子核素形状演化的研究

利用形变约束的相对论平均场理论系统研究了N=60同中子核素的形状演化, 给出了这些核的基态结合能、 形变、 单粒子能级以及形变激发的位能曲线。 通过比较和分析发现, 随着质子数的增加, N=60同中子核的基态形变向轴对称形变方向演化, 114Xe和116Ba位于球形U（5）和轴对称SU（3）的过渡区, 存在形状相变的临界点结构, 这些结果与实验观测一致。 The shape phase transition between spherical U（5）and axially SU（3）deformed nuclei is investigated systemically for N=60 isotonic chain by the constrained relativistic mean|field theory with the interactions NL3 and PK1. The values of bind energy and quadruple deformation β2 are calculated and a good agreement is obtained as compared with the experiments. By examining the potential energy curve and single particle spectra obtained with this microscopic approach, the possible critical point nuclei with the structure of shape phase transition are suggested to be 114Xe and 116Ba, which is favored by the experiments.     

Relativistic Charged Star Solutions in Higher Dimensions

We present a class of relativistic solutions of the Einstein-Maxwell equations for a spherically symmetric charged static fluid sphere in higher dimensions. The interior space at t=constant considered here possess (D?1) dimensional spheroidal geometry described by a higher dimensional Vaidya-Tikekar metric. A class of new static solutions of coupled Einstein-Maxwell equations is obtained in a D-dimensional space-time by prescribing the geometry of a (D?1) dimensional hyper spheroid in hydrostatic equilibrium. The solutions of the Einstein-Maxwell field equations are employed to obtain relativistic models for charged compact stars with a suitable law for variation of electric field in terms of the charged fluid content in the interior of the sphere. The central density is found to depend on the space-time dimensions and a physically realistic model is permitted for (D≥4). The validity of both Strong Energy Condition (SEC), Weak Energy Condition (WEC) are studied for a given configuration and compactness of compact objects. We found new class of solutions with interesting stellar models where it permits a star with a core having different property than the rest which however disappears in higher dimensions. The effect of dimensions on the Electric charge of the compact object is studied. We note that the upper limit of the electric field is determined by the space-time dimensions which are determined.     

Model of the Influence of Gravity-Wave Radiation from Relativistic Double Star Systems on the Electric Field in the Troposphere

Russian Physics Journal - A model is proposed to explain the observed influence of gravity waves of relativistic double stars on the vertical component of the Earth’s electric field in the...     

偶-偶超重核基态性质的理论研究

在形变的相对论平均场模型下采用NL Z2,TMA两套参数对一些偶 偶核基态性质进行了系统的计算,并将理论计算的结合能、α衰变能与已知的实验数据进行了对比分析.结果发现两方面的数据能够比较好地吻合,从而验证了相对论平均场模型对超重核研究是可行的.同时在计算中给出了未知核素基态性质的计算结果,可供以后在理论或实验上研究超重核时参考. The ground state properties of the even even nuclei with proton number Z=94-104 have been systematically calculated in the deformed relativistic mean field (RMF) theory with two sets of force parameters, TMA and NL Z2. Comparing the calculated binding energies and alpha decay energys with the experimental ones, it is found that theoretical results are in good agreement with experimental data. The reliability of the RMF model for even even superheavy nuclei has been tested by this comparison...     

相对论平均场理论对∧,Ξ和∑超核的研究(英文)

基于相对论平均场理论,系统地研究了单∧,Ξ和∑超核,超子-核子相互作用通过拟合实验数据以及参照之前理论工作来确定。以16O为核芯,通过加入不同类型超子（∧,Ξ0,-和∑+,0,-）,比较了超子的平均势场和单粒子能级,并研究了对核芯的杂质效应。整体上看,∧和Ξ0超子在大块性质上类似;Ξ0超子平均势场最浅;库仑相互作用对于带电超子Ξ-,∑+和∑-非常重要。作为杂质,原子核中加入超子会使整个体系更束缚。然而,不同超子对原子核的半径有不同效应。此外,讨论了ωYY张量耦合,发现其对超子的能级劈裂有显著影响,甚至导致Ξ超子中出现能级反转现象。Single ∧, Ξ, and ∑ hypernuclei are systematically studied within the framework of relativistic mean-field (RMF) model with YN interactions being constrained according to the experimental data and previous theoretical efforts. By adding a hyperon to 16O, the mean-field potentials and single-particle levels for hyperons (∧, Ξ0,-, and ∑+,0,-) are compared and the impurity effects on the nuclear core are examined. In general, the ∧ and ∑0 hyperons show similar behaviors in bulk properties since both of them are electroneutral and with similar coupling constants; Ξ0 hyperon owns the shallowest mean-field potential well; and Coulomb interactions play vital roles in the charged Ξ-, ∑-, and ∑+ hyperons. As an impurity, the intruded single-hyperon makes the nuclear system more bound in most cases due to the attractive NY interaction. However, very different effects on the nucleon radii are observed for different hyperons. Besides, the effects of the ωYY tensor couplings on the spin-orbit splitting are discussed, and remarkable influences are found which even change the level ordering of Ξ hyperon.     

A Class of Charged Relativistic Superdense Star Models

In this article we obtain a new class of well behaved charged solutions by using particular forms of the metric potential g ₄₄ and electric intensity, which involves a parameter K. The metric describing the superdense stars joins smoothly with the Reissner-Nordstrom metric at the pressure free boundary. This class of solutions describes well behaved charged fluid balls. The class of solutions gives range of parameter K (0.13≤K≤1.9999) for which the solution is well behaved hence, suitable for modeling of super dense star. The interior of the stars possess there energy density, pressure, pressure-density ratio and velocity of sound to be monotonically decreasing towards the pressure free interface. In view of the surface density 2×10¹⁴ gm/cm³, the maximum mass of the charged fluid balls and corresponding radius are 0.4711M _Θ and 7.0122 km. The red shift at the centre and boundary are found to be 0.1640 and 0.1100 respectively.