夸克物质中的色超导性理论简介

夸克-夸克通过单胶子交换的相互作用在其反对称态上是相互吸引的,在致密夸克物质里,这种吸引相互作用会导致费米面上的双夸克凝聚,这就是所谓的夸克配对或色超导现象。本文介绍了夸克配对或色超导现象的基本知识和一些新进展。色超导是一个对称性自发破坏现象,有非常丰富的破缺方式,我们介绍了色超导对称性及其自发破坏模式的分析方法,介绍了怎样计算色超导体两个最基本的变量：能隙和迈斯纳质量。然后我们介绍了描述色超导现象的有效理论。最后是这些理论的一个应用,即计算色超导体里的中微子发射率以及其它输运性质。本文可以作为研究夸克物质理论的入门参考资料。     

可能的qQ■，qq■■和qQ■■重四夸克态(英文)

假设X(3872)是一个qc(?)四夸克态,并用它的质量作为输入,用具有味对称性破坏的色磁相互作用系统研究了可能的重四夸克态的质量谱．     

可能的qQqQ,qqQQ和qQQQ重四夸克态

假设X(3872)是一个qcqc四夸克态, 并用它的质量作为输入, 用具有味对称性破坏的色磁相互作用系统研究了可能的重四夸克态的质量谱.     

电子型超导材料的超流密度响应

超导电性是凝聚态物理学中研究的热点.超导材料基本构成分为电子型与空穴型.对于空穴型超导材料,其电子配对对称性普遍接受的是具有dx2-y2波对称性;而对于电子型超导材料,电子配对对称性是dx2-y2波对称性还是s波对称性,目前还存在着很大的争议.在线性近似下,dx2-y2波超导体超流密度是温度的线性函数,而s波超导体的超流密度是温度的指数函数.因此通过对超流密度的研究可以明确电子型超导材料的电子配对对称性.本文首先从微观t-t′-t″-J模型出发,通过隶波色子平均场近似,计及反铁磁关联序和超导配对项,得到两带超导哈密顿量,进而推导出两带超流密度.最后验证了电子掺杂型超导体电子配对对称性和空穴掺杂型一样,同样具有dx2-y2波对称性,和早期唯象的两带模型的研究相一致.明确超流密度随掺杂的变化,是两带准粒子随掺杂变化相互作用的结果.     

世纪交替期物理学的两大困惑

 物质结构的新层次夸克禁闭相互作用的规范理论 电磁场相互作用的规范理论 扬米尔斯场对称性自发破缺 希格斯机制困惑与方向     

铁基超导材料超导能隙在不同费米面上分布的三维示意图

最近发现的高达55K铁基高温超导体结束了铜氧化物在超导转变温度高于40K的领域一统天下的局面.与铜氧化物高温超导体一样,超导配对对称性对于理解这一新的体系有着重要的作用.配对对称性包含超导能隙在动量空间的大小和相位信息,也就是打开超导电子对(库珀对)破坏超导在各个方向上所需要的能量,即电子对的结合能有多大,结合方向是什么,这些重要信息都能够从超导体的配对对称性中反映出来.     

手性ABM态p波超导体上临界磁场的角依赖关系

利用格林函数方法,通过Klemm-Clem变换,计算具有正交晶格结构椭球形费米面的手性ABM态p波超导体上临界磁场的角依赖关系.超导序参量选取具有手性ABM对称性的等自旋配对单分量形式.当椭球形费米面满足一定条件时,上临界磁场随角度呈现非单调变化,表明除配对电子有效质量的各向异性外,手性ABM态p波超导体也具有超导序参量的各向异性.计算结果可用于判断重费米子超导体Sr2RuO4的配对电子空间结构.     

物质结构在夸克-轻子层次上的动力学规律和研究发展趋势

文章综述了粒子物理中标准模型理论的历史发展、面临挑战以及未来的发展趋势.目前阶段物质结构最小组成单元是夸克和轻子,量子色动力学是描述夸克-胶子之间强相互作用的基本理论,它具有渐近自由和夸克禁闭的特点.量子色动力学和电弱统一理论一起构成粒子物理中标准模型理论.标准模型理论成功同时也面临两大挑战:对称性破缺的本质和夸克禁闭难题,这意味着标准模型理论需要发展和突破.人们期望粒子物理学、天文学和宇宙学交叉发展联手解决物质结构和早期宇宙研究中面临的难题,最终揭示超出标准模型的新物理规律.     

重费米子超导体的奇异特性

本文主要综述了最近几年对重费米子超导体CeCu_2Si_2、UBe_(13)和UPt_3所做的实验研究。着重介绍了重费米子超导体的奇异特性,尤其对与标准的BCS超导理论不符的实验现象和可能的P波配对超导的解释作了较系统的总结,对实验现象之间的一些关联也作了讨论。在理论方面,简要概述了对重费米子的起源、超导机制以及超导态的特性所做的理论研究的主要进展。     

重费米子超导体的奇异特性

本文主要综述了最近几年对重费米子超导体CeCu_2Si_2、UBe_(13)和UPt_3所做的实验研究。着重介绍了重费米子超导体的奇异特性,尤其对与标准的BCS超导理论不符的实验现象和可能的P波配对超导的解释作了较系统的总结,对实验现象之间的一些关联也作了讨论。在理论方面,简要概述了对重费米子的起源、超导机制以及超导态的特性所做的理论研究的主要进展。     

Quark condensation, induced symmetry breaking and color superconductivity at high density

The phase structure of hadronic matter at high density relevant to the physics of compact stars and relativistic heavy-ion collisions is studied in a low-energy effective quark theory. The relevant phases that figure are (1) chiral condensation, (2) diquark color condensation (color superconductivity) and (3) induced Lorentz-symmetry breaking (“ISB”). For a reasonable strength for the effective four-Fermi current–current interaction implied by the low-energy effective quark theory for systems with a Fermi surface we find that the “ISB” phase sets in together with chiral symmetry restoration (with the vanishing quark condensate) at a moderate density while color superconductivity associated with scalar diquark condensation is pushed up to an asymptotic density. Consequently, color superconductivity seems rather unlikely in heavy-ion collisions although it may play a role in compact stars. Lack of confinement in the model makes the result of this analysis only qualitative but the hierarchy of the transitions we find seems to be quite robust.     

Cooling of a compact star with LOFF matter core

Specific heat and neutrino emissivity due to direct URCA processes for quark matter in the color superconductive Larkin-Ovchinnikov-Fulde-Ferrell (LOFF) phase of Quantum-Chromodynamics have been evaluated. The cooling rate of simplified models of compact stars with a LOFF matter core is estimated. The text was submitted by the author in English.     

Neutrino Oscillation Induced by Chiral Phase Transition

Electric charge neutrality provides a relationship between chiral dynamics and neutrino propagation in compact stars. Due to the sudden drop of the electron density at the first-order chiral phase transition, the oscillation for low energy neutrinos is significant and can be regarded as a signature of chiral symmetry restoration in the core of compact stars.     

Superfluidity and superconductivity in the universe

The paper aims to elucidate the current status of the problem concerning the existence and observation of superfluid and superconducting states in the universe, that is, under cosmic conditions. Following an introduction, the paper discusses Bose-Einstein condensation, superfluidity, and superconductivity; possibilities for the occurrence of superfluidity and superconductivity under cosmic conditions; superconductivity of dense, degenerate electron plasma (large planets, white dwarfs); superfluidity and superconductivity in neutron stars; and finally superfluidity in a cosmological neutrino “sea.”     

Antikaon Condensation and In-medium Kaon and Antikaon Production in Protoneutron Stars

Antikaon condensation and kaon and antikaon production in protoneutron stars are investigated in a chiral hadronic model （also referred to as the FST model in this paper）. The effects of neutrino trapping on protoneutron stars are analyzed systematically. It is shown that neutrino trapping makes the critical density of K^- condensation delay to higher density and fifo condensation not occur. The equation of state （EOS） of （proto）neutron star matter with neutrino trapping is stiffer than that without neutrino trapping. As a result, the maximum masses of （proto）neutron stars with neutrino trapping are larger than those without neutrino trapping. If hyperons are taken into account, antikaon does not form a condensate in （proto）neutron stars. Meanwhile, the corresponding EOS becomes much softer, and the maximum masses of （proto）neutron stars are smaller than those without hyprons. Finally, our results illustrate that the Q values for K^＋ and K^- production in （proto）neutron stars are not sensitive to neutrino trapping and inclusion of hyperons.     

Effectively two-dimensional mechanism of axion and neutrino bremsstrahlung in the interaction of electrons with nuclei in a magnetic field

Axion and neutrino bremsstrahlung from electrons in the processes $e(Ze) \to e(Ze)a(\nu \bar \nu )$ is considered within the proposed two-dimensional covariant method for calculating Feynman diagrams in an external magnetic field. General expressions for squared matrix elements, as well as for the probability and power of this radiation, are obtained for a nonrelativistic nondegenerate electron gas. The energy scale f _a characteristic of the violation of global Peccei-Quinn symmetry is constrained by comparing the contributions of the above processes to the emissivity of magnetic neutron stars.     

强磁场中修正URCA过程的中微子产能率

基于n-p-e模型并考虑修正URCA过程中的质子分支,研究了强磁场对中子星核心区域修正URCA过程中微子产能率的影响.结果表明,强磁场使修正URCA过程的中微子产能率产生明显振荡;与中子分支相比,强磁场对质子分支中微子产能率的影响偏弱,但是它将提高总的中微子产能率.所得结论将有助于进一步研究中子星的冷却机理. 关键词： 中子星 强磁场 修正的URCA过程     

Magnetic color-flavor locking phase in high-density QCD

We investigate the effects of an external magnetic field in the gap structure of a color superconductor with three massless quark flavors. Using an effective theory with four-fermion interactions, inspired by one-gluon exchange, we show that the long-range component B of the external magnetic field that penetrates the color-flavor locked phase modifies its gap structure, producing a new phase of lower symmetry. A main outcome of our study is that the B field tends to strengthen the gaps formed by Q-charged and Q-neutral quarks that coupled among themselves through tree-level vertices. These gaps are enhanced by the field-dependent density of states of the Q-charged quarks on the Fermi surface. Our considerations are relevant for the study of highly magnetized compact stars.     

Color Superconductivity in Cold Dense Quark Matter

We investigate the phase structure of color superconducting quark matter at intermediate densities for two- and three-flavor systems. We thereby focus our attention on the influence of charge neutrality conditions as well as -equilibrium of the different phases. These constraints are relevant in the context of quark matter at the interior of compact stars. We analyze the implications of color superconductivity on compact star configurations using different hadronic and quark equations of state.Presented at the 15th Indian-Summer School of Physics: Understanding Dense Matter, Prague, Czech Republic, 27 August–1 September, 2003.