夸克介子模型的相图和表面张力

利用有限温度场论和平均场近似的方法,在考虑夸克真空涨落的情况下,研究了两个夸克味的夸克介子模型的量子色动力学相变的相图结构,得到了当夸克化学势密度较小时,量子色动力学相变是过渡相变,而当夸克化学势密度较大的时候,量子色动力学相变是一级相变.对于一级相变的区域,基于薄壁近似,给出了当温度等于临界温度Tc时,强子相表面张力随夸克化学势密度的变化关系.本研究为相对论重离子对撞实验和中子星早期结构演化提供必要的参考.     

化学非平衡夸克-胶子物质中等质量双轻子的产生

研究了正在进行化学平衡的富重子夸克-胶子物质的双轻子产生，发现由于产生在RHIC能量 的化学非平衡的富重子夸克-胶子物质冷却慢和高的初始温度，导致中等质量双轻子产生重 大增强.因此，中等质量双轻子的增强可以是夸克-胶子物质形成的信号.同时，这个增强能 补偿由于初始夸克化学势增加引起的双轻子抑制，因而双轻子产额的抑制不再是夸克-胶子 物质产生的信号. 关键词： 化学非平衡夸克-胶子物质 热粲夸克 双轻子     

化学非平衡夸克–胶子等离子体中的双轻子产生

研究了正在进行化学平衡的具有有限重子密度的夸克–胶子等离子体系统的演化和双轻子产生.结果发现由于夸克相的寿命随初始夸克化学势的增加而增加,以及其他一些因素,如较高的初始温度、较大的胶子密度和较大的胶子聚变和夸克湮没反应截面,导致热粲夸克对双轻子产生提供了占统治的贡献.这个效应造成中等质量双轻子的重大增强.     

平均场动力学与冷密夸克物质色导率

首先介绍了非Abel输运理论基础,然后在经典非Abel输运理论的基础上引入并评述了平均场动力学.作为应用,研究了有限化学势下冷密夸克物质系统的色动力学并计算出了色导率.最后比较了有限温度和有限化学势下的结果,讨论了其在天体物理领域的潜在价值.     

核子的部分子统计模型、EMC效应和核内核子中胶子分布函数

假定核子是部分子(夸克、胶子)组成的热力学系统,讨论了它的温度和化学势等热力学量,导出了核子中部分子的分数动量x分布与相应的统计分布间的关系式.通过将核子中胶子与黑体中光子的类比,计算了核子的有效温度.假定u、d夸克的化学势相同并取合理值,再利用重标度方案定出核内核子温度的改变后,统计模型很好地解释了EMC效应.认为胶子有小而负的化学势后,统计模型也较好地解释了虚光生J/ψ过程中束缚核子的与自由核子的胶子分布比值在小x处"过大"的问题.     

同位旋非对称强作用物质状态方程及热力学性质

在Nambu-Jona-Lasinio模型框架下,研究温度和重子化学势对同位旋非对称量子色动力学物质状态方程和热力学性质的影响.通过将零温和零重子化学势下的pion超流物质状态方程以及有限温下同位旋密度、压强与格点数据做比较,发现两种方法给出的结果符合得较好.进一步计算表明,零温和零重子化学势下的平均同位旋能量随同位旋密度单调增加,而非零重子化学势和有限温下却呈现具有极小值的非对称抛物线行为.最后,利用得到的状态方程探讨声速随同位旋化学势的变化行为,结果显示有限温和(或)重子化学势下的声速在相变点不连续,且超流相中的声速饱和值明显大于普通核物质及夸克物质中的值.另外,在超流相中重子化学势和温度具有软化状态方程以及降低声速的作用.     

强子化过程的手征奇异性质

基于Nambu-Jona-Lasinio(NJL)模型讨论了有限温度､有限密度下的强子化过程,考虑夸克-反夸克对转换成两个介子的情形,其微分散射截面作为质心系能量s,温度T和化学势的函数被计算到1/N_c展开的第一阶.着重考察有限密度情形手征对称性对强子化过程的影响.     

顶夸克为什么这么重?

 在费米实验室Tevatron质子-反质子对撞机上的CDF实验得到了第六味夸克(顶夸克)存在的证据(今年三月份,D0和CDF实验组同时宣布他们观测到了顶夸克--译者注),它使大家的注意力集中到了标准模型中的粒子的不寻常质量模式上。标准模型包含有三对夸克、三种带电轻子(电子、μ子和τ轻子)和其对应的三种中微子。夸克之间通过胶子“场”进行相互作用,同时也进行弱电相互作用。     

3到3的部分子弹性散射和早期热平衡化

研究了三胶子弹性散射ggg→ggg和三夸克弹性散射qqq→qqq. 证明了包含3→3弹性散射的输运方程的H定理. 输运方程给出了胶子物质热平衡化时间短和夸克物质热平衡化时间长的结果.     

夸克模型与等效的单介子交换N-N相互作用

利用夸克-反夸克产生模型推出了等效的单介子交换且包含顶点形状因子的N-N相互作用势, 结果在中长程部分与唯象相互作用符合较好.     

Spherical Symmetric Perfect Fluid Collapse in <Emphasis Type="Italic">f</Emphasis>(<Emphasis Type="Italic">R</Emphasis>, <Emphasis Type="Italic">T</Emphasis>) Gravity

This paper contains the study of spherically symmetric perfect fluid collapse in the frame work of f(R, T) modified theory of gravity. We proceed our work by considering the non-static spherically symmetric background in the interior and static spherically symmetric background in the exterior regions of the star. The junction conditions between exterior and interior regions are presented by matching the exterior and interior regions. The field equations are solved by taking the assumptions that the Ricci scalar as well as the trace of energy-momentum tensor are to be constant, for a particular f(R, T) model. By inserting the solution of the field equations in junction conditions, we evaluate the gravitational mass of the collapsing system. Also, we discuss the apparent horizons and their time formation for different possible cases. It is concluded that the term f(R ₀, T ₀) behaves as a source of repulsive force and that’s why it slowdowns the collapse of the matter.     

Strange stars in <Emphasis Type="Italic">f</Emphasis>(<Emphasis Type="Italic">R</Emphasis>) theories of gravity in the Palatini formalism

In the present work we study strange stars in f(R) theories of gravity in the Palatini formalism. We consider two concrete well-known cases, namely the \(R+R^2/(6 M^2)\) model as well as the \(R-\mu ^4/R\) model for two different values of the mass parameter M or \(\mu \). We integrate the modified Tolman–Oppenheimer–Volkoff equations numerically, and we show the mass-radius diagram for each model separately. The standard case corresponding to the General Relativity is also shown in the same figure for comparison. Our numerical results show that the interior solution can be vastly different depending on the model and/or the value of the parameter of each model. In addition, our findings imply that (i) for the cosmologically interesting values of the mass scales \(M,\mu \) the effect of modified gravity on strange stars is negligible, while (ii) for the values predicting an observable effect, the modified gravity models discussed here would be ruled out by their cosmological effects.     

"Ultracold" neutral plasmas at room temperature

We report a measurement of the electron temperature in a plasma generated by a high-intensity laser focused into a jet of neon. The 15?eV electron temperature is determined using an analytic solution of the plasma equations assuming local thermodynamic equilibrium, initially developed for ultracold neutral plasmas. We show that this analysis method accurately reproduces more sophisticated plasma simulations in our temperature and density range. While our plasma temperatures are far outside the typical "ultracold" regime, the ion temperature is determined by the plasma density through disorder-induced heating just as in ultracold neutral plasma experiments. Based on our results, we outline a pathway for achieving a strongly coupled neutral laser-produced plasma that even more closely resembles ultracold neutral plasma conditions.     

基尔霍夫定律中的“独立回路”

对电路理论基尔霍夫定律中“独立回路”概念进行讨论,提出较为合理的独立回路的概念,并运用线性代数、几何方法、拓扑图论等方法,分别对平面电路网络和立体电路网络进行讨论,证明在此规定下基尔霍夫方程的独立性和解的确定性.     

Equations of fluctuating nonlinear hydrodynamics for normal fluids

The full set of fluctuating nonlinear hydrodynamic equations for normal fluids is derived from the conventional Langevin equations extended to include multiplicative noise. The equations describing the set of conserved variables (the mass density, the momentum densityg, the energy density) agree with those found by Morozov for a case of a driving free energy which is a local function of the hydrodynamic variables. We show here that if the standard form of the hydrodynamic equations is to hold in the absence of noise, then the driving free energy must be a local function ofg and, but it may have to be a nonlocal function of the mass density.     

Evolution of wave turbulence under "gusty" forcing

We consider nonlinear evolution of a random wave field under gusty forcing, fluctuating around a constant mean. Here the classical wave turbulence theory that assumes a proximity to stationarity is not applicable. We show by direct numerical simulation that the self-similarity of wave field evolution survives under fluctuating forcing. The wave field statistical characteristics averaged over fluctuations of forcing evolve as if there were a certain constant "effective wind." The results justify the use of the kinetic equations with forcing averaged over gusts as a good first approximation.     

Tensorial representation of the Dirac equation

We discuss tensor representations of the Dirac equation using a geometric approach. We find that the mass zero Dirac equations can be represented by Maxwell equations having a source which obeys the empty space wave equation. We also obtain a relation for the source in terms ofE andH. In the case of mass not equal to zero a difficulty is encountered in removing the constant spinors¯ _Aand¯ _A.We find that the arbitrary constant spinors can be eliminated in a spinor theory based on the Klein-Gordon equation.     

General relativistic effects in the structure of massive white dwarfs

In this work we investigate the structure of white dwarfs using the Tolman–Oppenheimer–Volkoff equations and compare our results with those obtained from Newtonian equations of gravitation in order to put in evidence the importance of general relativity (GR) for the structure of such stars. We consider in this work for the matter inside white dwarfs two equations of state, frequently found in the literature, namely, the Chandrasekhar and Salpeter equations of state. We find that using Newtonian equilibrium equations, the radii of massive white dwarfs (\(M>1.3M_{\odot }\)) are overestimated in comparison with GR outcomes. For a mass of \(1.415M_{\odot }\) the white dwarf radius predicted by GR is about 33% smaller than the Newtonian one. Hence, in this case, for the surface gravity the difference between the general relativistic and Newtonian outcomes is about 65%. We depict the general relativistic mass–radius diagrams as \(M/M_{\odot }=R/(a+bR+cR^2+dR^3+kR^4)\), where a, b, c and d are parameters obtained from a fitting procedure of the numerical results and \(k=(2.08\times 10^{-6}R_{\odot })^{-1}\), being \(R_{\odot }\) the radius of the Sun in km. Lastly, we point out that GR plays an important role to determine any physical quantity that depends, simultaneously, on the mass and radius of massive white dwarfs.     

Gravitational and Electroweak Unification

Einstein suggested that a unified field theorybe constructed by replacing the diffeomorphisms (thecoordinate transformations of general relativity) withsome larger group. We have constructed a theory that unifies the gravitational and electroweakfields by replacing the diffeomorphisms with the largestgroup of coordinate transformations under whichconservation laws are covariant statements. Thisreplacement leads to a theory with field equations whichimply the validity of the Einstein equations of generalrelativity, with a stress-energy tensor that is justwhat one expects for the electroweak field andassociated currents. The electroweak field appears as aconsequence of the field equations (rather than as a"compensating field" introduced to secure gaugeinvariance). There is no need for symmetry breaking toaccommodate mass, because the U(1) × SU(2) gaugesymmetry is approximate from the outset. Thegravitational field is described by the space-timemetric, as in general relativity. The electroweak fieldis described by the "mixed symmetry" part of the Riccirotation coefficients. The gauge symmetry-breakingquantity is a vector formed by contracting theLevi-Civita symbol with the totally antisymmetric partof the Ricci rotation coefficients.     

"Weighing" a closed system and the time-energy uncertainty principle

A gedanken experiment is proposed for "weighing" the total mass of a closed system from within the system. We prove that for an internal observer the time tau, required to measure the total energy with accuracy DeltaE, is bounded according to tauDeltaE>Planck's over 2pi. This time-energy uncertainty principle for a closed system follows from the measurement backreaction on the system. We generally examine what other conserved observables are in principle measurable within a closed system and what are the corresponding uncertainty relations.