磁场中夸克物质的非轻子弱作用过程

讨论了磁场中夸克物质的非轻子弱作用过程. 改进了在弱磁场情况下的近似计算方法, 分别给出了强弱磁场下非轻子过程的反应率的表达式, 以及一定条件下的近似表达式. 结果显示, 强磁场极大的抑制反应率的大小, 进而影响奇异夸克物质的粘滞性.     

奇异物质体黏滞系数的计算和奇异星振动的阻尼

利用与奇异夸克质量相关的非轻子弱过程u+s←→d+u的反应速率, 在考虑了夸克之间的相互作用并做了热力学自恰处理后, 重新推导、计算了奇异夸克物质的体黏滞系数. 由于热力学自恰的需要引入一项压力附加项, 使得奇异星的体黏滞系数比前人计算的有了很大的增加. 通过计算振动衰减时间我们发现, 虽然体黏滞系数增大了很多, 但以前对于奇异星观测的结论仍然成立.     

胶子非弹性散射过程对夸克胶子等离子体中双轻子产生的影响

双轻子是研究夸克物质的形成和性质的重要探针.本文基于化学平衡化的黏滞性夸克胶子等离子体演化模型,计算了相对论重离子碰撞能量下金-金对心碰撞形成的夸克胶子等离子体中的双轻子产额.在黏滞性计算中加入了胶子非弹性散射过程对黏滞系数的贡献.相较仅考虑夸克和胶子弹性散射的情况,双轻子的产额有较明显的降低.这表明在黏滞系数中加入胶子非弹性散射的贡献使得系统的演化过程加快,演化时间变短.     

膨胀的热夸克胶子物质的中等质量双轻子的增强

基于一个描述夸克胶子火柱演化的相对论流体力学模型,研究了夸克相、强子相互作用以及非热过程(DrellYan对、粲强子衰变)的中等质量双轻子的产生.发现由于相边对夸克胶子物质演化的影响和RHIC能量核碰撞产生的夸克胶子物质具有高的初始温度,夸克相对双轻子的贡献显著增强,比那些来自强子相互作用的贡献重要,甚至能与来自非热的贡献比较.表明中等质量双轻子的增强是一个在核碰撞中产生了夸克胶子物质的可能信号. 关键词： 夸克-胶子物质 双轻子增强 相对论流体力学模型     

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     

只带一种基本标量粒子的轻子-夸克复合模型

我们提出一个包括两种基本费米子和一种基本标量粒子的轻子-夸克复合模型. 其中, 基本费米子无质量并且不带色, 基本标量粒子是色的三重态. SU(3)_H定域规范作用将基本粒子束缚成轻子、夸克和弱玻色子等复合粒子. 轻子是由三个基本费米子组成的三体复合粒子, 夸克由一个基本费米子和一个基本标量粒子组成. 本模型基本粒子的数目较少, 存在为数不多的exotic粒子. 解释了轻子-夸克的对称性. 弱作用是超色单态之间的一种短距剩余作用, 它只在复合层次出现. 通过动力学对称破缺破坏了宇称守恒.     

一个具有三代家族的夸克和轻子的复合模型

为了解释家族问题,本文提出了一个具有SU(3)_sc×SU(6)规范对称的夸克和轻子的复合模型.组成夸克和轻子的成份(preon)是两类无质量自旋为1/2的费米子.运用费米原理于超色单态的preon复合体系,可以产生与实验观测以及宇宙大爆炸理论预言符合的三代轻的夸克和轻子家族.弱玻色子也是由同一组preon组成的复合粒子.弱相互作用不是preon层次的基本相互作用.在preon能标,没有质子衰变的困难.     

关于Reggeon的结构

从强子组分夸克具有结构的观点出发，根据高能强作用软过程中的最大非微扰强作用反应假定,提出了关于Reggeon(IR)的结构模型.高能时对撞强子中的一对组分夸克-反夸克在最大反应下有一定的几率先分解为非微扰胶子和旋量团(反旋量团).此旋量团对将进一步演化而放射出一系列的非微扰胶子(和夸克对)并最终湮没.将这种过程与其逆向(厄米共轭)过程并合,就可得出有关的IR的场论结构图象.它是以旋量团为竖线,胶子为横线的一系列切割梯形图之和所代表.本文在系统能量大而动量转移很小的多重Regge运动学区间和只保留Ins的领头阶近似下,计算了这组切割梯形图相应的散射振幅,求出了它们的总和,得出了与轻夸克介子对应的典型Regge极点轨迹的简洁表达式,对结果进行了简单的讨论.     

QCD非微扰和能量丢失效应对夸克分布影响

在非常数性K因子的情况下,根据核Drell-Yan过程的高能强子h同原子核A碰撞和高能轻子l同原子核A深度非弹性碰撞的实验数据,在考虑QCD非微扰效应对深度非弹性散射部分子分布的影响及Drell-Yan过程中的能量丢失效应,计算确定价夸克分布和海夸克分布核效应函数RAυ(x₂),RAS(x₂)的变化,深化了对原子核内夸克分布受核效应影响的认识     

强子作为非拓扑孤粒子的SU(5)大统—模型(Ⅰ)

提出一种新的包含三代已知轻子与夸克的SU(5)大统—模型.按本模型,强子可看作由夸克形成的非拓扑孤粒子;轻子与夸克本质上是相同的,它们之间的差别是由对称性自发破缺造成的;在强子内部,夸克质量很小,其性质与已知夸克相同;在强子外部,夸克的性质与已知轻子相同,只是质量很重,并将很快衰变.本文除了定义严格守恒的电荷Q0、费米子数F0外,还在孤粒子内部定义了近似守恒的内色荷、内电荷、内费米子数.已知SU(5)大统—模型的(L-B)守恒相应于本模型的F0守恒.     

高温近似下奇异夸克物质的体粘滞系数

在准粒子描述下,采用自洽的热力学方法,考虑奇异夸克物质(SQM?)的介质效应,计算了高温近似下奇异夸克物质的体粘滞系数.发现介质效应对奇异夸克物质的体粘滞系数有很大影响,这使得观测数据不再排除两味色超导相奇异星的存在.     

Constituent quark model for baryons with strong quark-pair correlations and non-leptonic weak transitions of hyperon

We study the roles of quark-pair correlations for baryon properties, in particular on non-leptonic weak decay of hyperons. We construct the quark wave function of baryons by solving the three body problem explicitly with confinement force and the short range attraction for a pair of quarks with their total spin being 0. We show that the existence of the strong quark-quark correlations enhances the non-leptonic transition amplitudes which is consistent with the data, while the baryon masses and radii are kept to the experiment.     

SU(3) as gauge group of the vectorlike weak and electromagnetic interactions

A scheme of the weak and electromagnetic interactions based on the group SU(3) as well as on six quark flavours and eight leptons is presented. Several aspects of the weak interactions are discussed, in particular the presence of new right-handed currents, the neutral current, the generation of the Cabibbo angle, and the dominant non-leptonic weak interaction.     

Strange Quark Matter and Strangelets in a Strong Magnetic Field

We study the stability properties of magnetized strange quark matter and strangelets under a strong magnetic field in the MIT bag model. The free energy per baryon of strange quark matter feels a great influence from the magnetic field. At the field strength about 10¹⁷G, the magnetized strange quark matter becomes more stable. Considering the finite size effect, the magnetic influence on strangelets becomes complicated. For a given magnetic field, there exists a critical baryon number, below which the magnetized strangelets have lower energy than the non-magnetized strangelets. For the field strength of 5× 10¹⁷G, the critical baryon number is A_c ～ 100. Generally, the critical baryon number increases with the decreasing external magnetic field. When the field strength is smaller than 10¹⁷G, the critical baryon number goes up to A_c～ 10⁵. The stable radius, electric charge, and quark flavor fractions of magnetized strangelets are shown.     

Strange matter at finite temperatures

The properties of strange quark matter at finite temperatures and in equilibrium with respect to weak interaction are explored on the basis of the MIT bag model picture of QCD. Furthermore, to determine the stability of strange quark matter, analogous investigations are also performed for nuclear matter within Walecka's model field theory. It is found that strange quark matter can be stable at zero external pressure only for temperatures below 20 MeV. The existence of this limiting temperature is a consequence of the Van der Waals like behaviour of nuclear matter at low temperatures.     

Bulk viscosity of hot dense Quark matter in the PNJL model

Starting from the Kubo formula and the QCD low energy theorem, we study the the bulk viscosity of hot dense quark matter in the PNJL model from the equation of state. We show that the bulk viscosity has a sharp peak near the chiral phase transition, and that the ratio of bulk viscosity over entropy rises dramatically in the vicinity of the phase transition. These results agree with those from the lattice and other model calculations. In addition, we show that the increase of chemical potential raises the bulk viscosity.     

Neutron star in the presence of strong magnetic field

Compact stars such as neutron stars (NS) can have either hadronic or exotic states like strange quark or colour superconducting matter. Stars can also have a quark core surrounded by hadronic matter, known as hybrid stars (HS). The HS is likely to have a mixed phase in between the hadron and the quark phases. Observational results suggest huge surface magnetic field in certain NS. Therefore, we study here the effect of strong magnetic field on the respective equation of states (EOS) of matter under extreme conditions. We further study the hadron–quark phase transition in the interiors of NS giving rise to HS in the presence of strong magnetic field. The hadronic matter EOS is described based on RMF theory and we include the effects of strong magnetic fields leading to Landau quantization of the charged particles. For quark phase, we use the simple Massachusetts Institute of Technology (MIT) bag model, assuming density-dependent bag pressure and magnetic field. The magnetic field strength increases from the surface to the centre of the star. We construct the intermediate mixed phase using Glendenning conjecture. The magnetic field softens the EOS of both the matter phases. We finally study, the mass–radius relationship for such types of mixed HS, calculating their maximum mass, and compare them with the recent observations of pulsar PSR J1614-2230, which is about 2 solarmass.     

Theu+d ↔u+s reaction rate and bulk viscosity of strange matter

The influence of the strong interactions in strange matter on its nonleptonic reaction rate and bulk viscosity is studied. We find the rate is strongly suppressed by these interactions. The bulk viscosity is also influenced by them. At low temperatures, the viscosity is strongly suppressed; but at high temperatures, it is slightly enhanced. The astrophysical implications of these results are also discussed.     

Bulk viscosity of strange quark matter in density dependent quark mass model

We have studied the bulk viscosity of strange quark matter in the density dependent quark mass model (DDQM) and compared results with calculations done earlier in the MIT bag model where u, d masses were neglected and first order interactions were taken into account. We find that at low temperatures and high relative perturbations, the bulk viscosity is higher by 2 to 3 orders of magnitude while at low perturbations the enhancement is by 1–2 order of magnitude as compared to earlier results. Also the damping time is 2–3 orders of magnitude lower implying that the star reaches stability much earlier than in MIT bag model calculations.