利用非对称核物质状态方程对中子星的质量和半径的研究

在温度、密度及同位旋相关的核物质状态方程的基础上,通过求解Tol-man-Oppenheimer?Volkoff方程得到了中子星的质量与中心密度的关系,发现随着中心密度的变化,中子星存在一个最大质量.同时计算结果表明,中子星的最大质量与核物质状态方程的不可压缩系数、有效质量及对称能强度系数等密切相关.对中子星半径的研究表明,较硬的核物质状态方程给出的中子星半径较大,而且较大的对称能强度系数和较大的核子有效质量也会给出较大的中子星半径.     

同位旋激发能研究

在扩展的Skyrme有效相互作用下,利用Hartree-Fock理论研究了同位旋激发能与温度、密度的关系.结果表明同位旋激发能随密度的降低以及温度的增加而降低.同时研究了对称能与同位旋激发能的关系,指出对称能是同位旋激发能的一部分,且占相当大的比重.最后研究了不同的势参数下,同位旋激发能随相对中子过剩的变化关系,发现同位旋激发能较强地依赖于对称能强度系数,而对不可压缩系数以及有效质量不太敏感.从而为实验上通过研究同位旋激发能来提取核物质状态方程中的对称能部分指出了一条途径.     

核物质对称能斜率对快转中子星性质的约束（英文）

在过去的十余年中,对非对称核物质的对称能的研究无论从实验还是理论上都取得了较大的突破,这对中子结构及其物态方程的理解具有十分重要的意义。本研究将采用一个相对保守的对称能斜率范围(25 Me VL105Me V)来研究其对快速转动中子星性质的约束,这些性质包括:质量-半径关系、转动惯量、引力红移以及转动形变等。通过该对称能斜率的约束,发现典型中子星(M=1.4M⊙)的半径约束在10.28～13.43 km范围内,这与最近的相关观测相一致。如果观察发现了质量较小的毫秒脉冲星,则将为核物质的对称能较软提供有效的证据。另外还发现,对角动量的一致性可为快转中子星转动惯量的上限提供约束。最后,根据具有低质量伴星的双星EXO0748-676的红移观测,给出了该脉冲星的质量下限(1.5M⊙)。     

多重碎裂的同位旋效应和动量相关作用的影响

利用同位旋相关的量子分子动力学模型,对中能重离子碰撞过程中多重碎裂对于同位旋自由度和动量相关作用的依赖性进行了研究.结果表明:在相对较高能区,碎片的平均多重性敏感地依赖于介质中核子–核子碰撞截面的同位旋效应,但很弱地依赖于对称势;动量相关作用增强了中等质量碎片多重性对于核子–核子碰撞截面的同位旋依赖的敏感性.中等质量碎片的平均多重性可用作提取介质中同位旋相关的核子–核子碰撞截面的探针.     

低SIS能区重离子碰撞过程的系统性研究

在极端相对论量子分子动力学(UrQMD)模型中加入势能密度泛函形式的势修正、核子-核子弹性散射截面的更细致的介质修正以及碎片重构模式中的同位旋效应后,重点研究低SIS能区(约40～400 MeV/u)重离子碰撞的动力学过程。在较系统地研究此能区重离子碰撞后的轻碎片产生及集体流后,重点研究对高密区对称能密度依赖敏感的观测量。发现:(1)质量对称的Sn系列同位素反应系统,其中子平衡能的系统N/Z分布能敏感探测对称能密度依赖;(2)横速度/动量分布的中子和质子及氢同位素的椭圆流比vn2/vp,H2敏感依赖于对称能。经采用多组核物质标量不可压缩系数K0值差别很小、对称能斜率参数L值相差较大的Skyrme势参数计算并对FOPI/LAND相应数据做χ2分析后抽取的L值为(89±45)MeV。     

σ介子的自相互作用对核物质物态方程的影响

在相对论σ–ω模型里,详细讨论了σ介子的自相互作用参数对正常核物质物态方程的影响,特别是对核物质的不可压缩系数、有效质量,以及σ介子与核子、ω介子与核子之间的耦合常数的影响,发现这些参数与核物质的性质之间有紧密的联系.同时,利用这些结果研究了相对论σ–ω–π模型下△共振态核物质的结合能和压强与温度之间的关系,并同我们以前的结果作了比较,得到了一些有意义的结果.在以上所有的分析中,考虑了核子、△粒子和σ介子的真空起伏.     

重离子碰撞中原子核阻止的同位旋效应

利用含有3种对称势形式的同位旋相关的量子分子动力学,研究了中能重离子碰撞中原子核阻止的同位旋效应和随入射道条件的系统演化过程.计算结果表明,原子核阻止灵敏地依赖束流能量、碰撞参数、碰撞系统的质量和核子–核子碰撞截面的同位旋相关性,而3种对称势和碰撞系统的中质比对它的影响不很明显,但在大约费米能量以下能区,原子核阻止同时依赖于介质中核子–核子碰撞截面和对称势.故认为在费米能量以上能区直至150MeV/u,原子核阻止是提取介质中核子–核子碰撞截面的一个新的物理观测量.     

自洽的相对论微观光学位研究

在Dirac-Brueckner计算由于忽略负能态引起解的不唯一性可以根据Hugenholtz-Van Hove定理,要求核物质在饱和密度处每个核子的分离能等于费米能来给出限制.选取核子饱和结合能为E_B/A=－15.8MeV,自洽计算得到核物质的饱和密度k_f=1.41fm^－1以及有效质量为m*/m=0.52,核的不可压缩系数K=280MeV.利用热力学第一定律可以得到自洽的有效质量(实的标量位)和每个核子的平均结合能随核密度的分布,采用现实的核子-核子相互作用的Bonn位,解RBBG方程得到核在介质中的矢量位,它与动量的依赖关系是很弱的.用这种新的自洽的相对论微观光学位我们进一步讨论了核子-核散射的微分截面和自旋观测量.     

中子星中质子比例的密度依赖

利用Hartree-Fock理论,基于扩展的Skyrme有效相互作用,采用抛物线近似下对称能的密度相关形式以及β平衡和电中性条件,给出了中子星中质子比例的密度依赖关系.通过比较不同的势参数SII,SIII,SKM和SKI5下对称能强度系数的密度依赖关系研究了中子星中的质子比例,发现在高密时势参数SII,SIII和SKM能够给出中子星中质子消失的结果,这预示着致密核物质可能存在纯中子物质的基态.同时计算表明,考虑中子星中μ^－子的贡献后使质子比例增加.     

中子星对自旋相关轴矢量新相互作用的约束

众多粒子物理超标准模型中都预言了自旋有关的新相互作用存在.极化的核子间通过交换自旋为1的轴矢量玻色子可以产生额外的吸引力进而改变无穷大核物质状态方程性质.本文在相对论平均场模型的框架下加入额外的轴矢量玻色子后计算发现,当相互作用强度与玻色子质量之比达到g_A~2/m_(Z′)~2～O(10 GeV~(-2))时,低密处无穷大核物质的稳定性和对应的相变行为将发生显著的改变;而当g_A~2/m_(Z′)~2 130 GeV~(-2)时核物质将在发生相变前率先到达零压点.对中子星而言这意味着其内核物质将在保持稳定的状态下形成表面而不会发生相变形成壳层结构,这与普遍存在于中子星天文观测中的星震现象矛盾,因此反过来对新相互作用的强度提出了额外的限制.通过与已有的地面实验结果对比,本文发现对于力程为微米到厘米间的新相互作用,中子星对其强度的约束最高可有8个量级的提升.     

Properties of hyperon stars rotating at Keplerian frequency

The structure and properties of a Keplerian rotating hyperon star with an equation of state (EOS) investigated using the relativistic σ--ω--ρ model are examined by employing an accurate numerical scheme. It is shown that there is a clear rotating effect on the structure and properties, and that hyperon star matter cannot support a star with a mass larger than 1.9 M_Θ, even a star rotating at the fastest allowed frequency. The constraints of the two known fastest rotating frequencies (716 Hz and 1122 Hz) on the mass and radius of a hyperon star are also explored. Furthermore, our results indicate that the imprint of the rapid rotation of a hyperon star on the moment of inertia is clear; the backward equatorial redshift, the forward equatorial redshift and the polar redshift can be distinguished clearly, the forward equatorial redshift is always negative; and its figuration is far from a spherical symmetric shape.     

Influence of the weakly interacting light U boson on the properties of massive protoneutron stars

Considering the octet baryons in relativistic mean field theory and selecting entropy per baryon S=l,we calculate and discuss the influence of U bosons on the equation of state,mass-radius,moment of inertia and gravitational redshift of massive protoneutron stars(PNSs).The effective coupling constant gu of U bosons and nucleons is selected from 0 to 70 GeV~(-2).The results indicate that U bosons will stiffen the equation of state(EOS).The influence of U bosons on the pressure is more obvious at low density than high density,while the influence of U bosons on the energy density is more obvious at high density than low density.The U bosons play a significant role in increasing the maximum mass and radius of PNS.When the value of gu changes from 0 to 70 GeV~(-2),the maximum mass of a massive PNS increases from 2.11M_⊙ to 2.58M_⊙,and the radius of a PNS corresponding to PSR J0348+0432 increases from 13.71 km to 24.35 km.The U bosons will increase the moment of inertia and decrease the gravitational redshift of a PNS.For the PNS of the massive PSR J0348+0432,the radius and moment of inertia vary directly with gu,and the gravitational redshift varies approximately inversely with gu.     

Slowly rotating neutron stars and hadronic stars in the chiral SU(3) quark mean-field model

The equations of state for neutron matter, strange and non-strange hadronic matter in the chiral SU(3) quark mean-field model are applied in the study of slowly rotating neutron stars and hadronic stars. The radius, mass, moment of inertia, and other physical quantities are carefully examined. The effect of the nucleon crust for the strange hadronic star is exhibited. Our results show that the rotation can increase the maximum mass of compact stars significantly. For a big enough mass of pulsars which cannot be explained as strange hadronic stars, theoretical approaches to increase the maximum mass are addressed.     

Hyperon coupling dependence of hadron matter properties in relativistic mean field model

The properties of hadronic matter at β equilibrium in a wide range of densities are described by appropriate equations of state in the framework of the relativistic mean field model. Strange meson fields, namely the scalar meson field σ＊（975） and the vector meson field φ（1020）, are included in the present work. We discuss and compare the results of the equation of state, nucleon effective mass, and strangeness fraction obtained by adopting the TM1, TMA, and GL parameter sets for nuclear sector and three different choices for the hypcron couplings. We find that the parameter set TM1 favours the onset of hyperons most, while at high densities the GL parameter set leads to the most hyperon-rich matter. For a certain parameter set （e.g. TM1）, the most hyperon-rich matter is obtained for the hyperon potential model. The influence of the hyperon couplings on the effective mass of nucleon, is much weaker than that on the nucleon parameter set. The nonstrange mesons dominate essentially the global properties of dense hyperon matter. The hyperon potential model predicts the lowest value of the neutron star maximum mass of about 1.45 Msun to be 0.4--0.5 Msun lower than the prediction by using the other choices for hyperon couplings.[第一段]     

包含暗物质的强子夸克混合星

研究了含有暗物质的夸克核心混合星的观测属性。用相对论平均场理论和有效质量口袋模型分别描述夸克核心的混合星物质内强子相和夸克相,用Gibbs相平衡条件描述强子-夸克混合相,研究了由于包含强、弱相互作用的费米子暗物质对混合星质量、半径、引力红移、自转频率和转动惯量等整体观测属性的影响。结果表明,在强、弱相互作用下,暗物质粒子质量大于等于0.5 GeV时暗物质会使混合星的状态方程比无暗物质时有一定软化,相应的混合星最大质量减少。当调节暗物质粒子质量研究表明,随着暗物质粒子质量的增大,夸克核心的混合星物质的状态方程变软,混合星的质量、半径变小,并且引力红移、自转频率和转动惯量等整体观测属性也明显依赖于暗物质粒子的质量。当暗物质粒子质量0.1 GeV时,包含强、弱作用暗物质的混合星质量达到2.0 M_⊙和2.8 M_⊙（其中M_⊙为太阳质量）,说明大质量脉冲星PSR J1859-0131和J1931-01可能是包含小质量暗粒子暗物质的强子夸克的混合星。整体观测属性的计算结果均在中子星的天文观察数据范围内,也说明强子夸克的混合星内可能包含暗物质。The observational properties of quark core hybrid star contain dark matter are studied. The influences of containing of strongly or weakly interacting dark matter to global observational features of hybrid stars, mass, radius, gravitational red-shift, rotational period and moment of inertia are studied by using relativistic mean field theory to describe hadron phase, effective mass bag model to quark phase, and Gibbs phase equilibrium conditions to hadron-quark mixed phase respectively. Our results indicate that, both in the strong and weak interacting case, the equation of state for hybrid star matter contain dark matter become softer than that of without dark matter while the mass of dark matter particles larger than 0.5 GeV, which leads to the decrease of the mass and corresponding radius of hybrid star. With the increase of the dark matter particle mass, the equation of state for hybrid star matter become softer, this cause the decrease of the mass and radius of hybrid star obviously. The gravitational red-shift and the rotational period, obviously increase of the moment of inertia of the hybrid stars are influenced by the dark matter particle mass. When the dark matter particle mass is equal to 0.1 GeV, the masses of the star with strong and weak interacting dark matter reach to 2.0 M_⊙ and 2.8 M_⊙(M_⊙ is the solar mass), this result indicates that the giant mass PSR, J1859-0131 and J1931-01, can be a hadron-quark hybrid star and containing dark matter with small dark particle mass. The computational results of all above global observational features of hybrid stars are in the range of astronomical observation data, these also indicate that hybrid star with quark core may contains dark matter.     

Thermal Dynamics Behavior of Protoneutron Star Matter

In the relativistic σ-ω model, including the vacuum fluctuation of nucleons and σ mesons, the effect of the temperature to the composition and equation of state of protoneutron star matter, nucleon effective mass and chemical potential of neutrons and electrons are studied. We find that the influence of the temperature on the equation of state of protoneutron star matter is indeed small, however, its influence on the composition of protoneutron star, which will contribute to the evolution of protoneutron star, cannot be neglected in low density region. The chemical potentials of neutrons and electrons also depend on the temperature in almost the same density region.     

Constraining the Surface Gravitational Redshift of Proto Neutron Stars with New Nucleon Coupling Constants

A new set of nucleon coupling constants (CZ11) is obtained for the relativistic mean field (RMF) theory based on the recent experimental information on the symmetry energy derived from the data from NSCL/MSU. The surface gravitational redshift of a proto neutron star (PNS) is examined within the RMF framework for the baryon octet system by using this set of parameters. It is found that the surface gravitational redshift for CZ11 is smaller than that for GL97. For the CZ11 parameter set, the surface gravitational redshift of a PNS at T=15 MeV is smaller than that at T=0 MeV. It is also found that the surface gravitational redshift corresponding to M _max/R for the CZ11 parameter set is smaller by about 10 percent than that for GL97, with M _max being the maximum mass and R being the corresponding radius.     

核物质和夸克物质的对称能（英文）

对称能表征了同位旋非对称强相互作用物质状态方程的同位旋相关部分,它对于理解核物理和天体物理中的许多问题有重要意义。简要总结了关于核物质和夸克物质对称能研究的最新进展。对于核物质对称能,通过对核结构,核反应以及中子星的研究,目前对其亚饱和密度的行为已有比较清楚的认识,同时,对饱和密度附近对称能的约束也取得了很好的研究进展。但如何确定核物质对称能的高密行为仍然是一个挑战。另一方面,在极端高重子数密度条件下,强相互作用物质将以退禁闭的夸克物质状态存在。同位旋非对称夸克物质可能存在于致密星内部,也可能产生于极端相对论重离子碰撞中。对最近关于夸克物质对称能对夸克星性质的影响以及重夸克星的存在对夸克物质对称能的约束的研究工作进行了介绍,结果表明同位旋非对称夸克物质中上夸克和下夸克可能感受到很不一样的相互作用,这对于研究极端相对论重离子碰撞中部分子动力学的同位旋效应有重要启发。The symmetry energy characterizes the isospin dependent part of the equation of state of isospin asymmetric strong interaction matter and it plays a critical role in many issues of nuclear physics and astrophysics. In this talk, we briefly review the current status on the determination of the symmetry energy in nucleon (nuclear) and quark matter. For nuclear matter, while the subsaturation density behaviors of the symmetry energy are relatively well-determined and significant progress has been made on the symmetry energy around saturation density, the determination of the suprasaturation density behaviors of the symmetry energy remains a big challenge. For quark matter, which is expected to appear in dense matter at high baryon densities, we briefly review the recent work about the effects of quark matter symmetry energy on the properties of quark stars and the constraint of possible existence of heavy quark stars on quark matter symmetry energy. The results indicate that the u and d quarks could feel very different interactions in isospin asymmetric quark matter, which may have important implications on the isospin effects of partonic dynamics in relativistic heavy-ion collisions.