D介子稀有衰变研究

利用工作在北京正负电子对撞机(BEPC)上的北京谱仪(BES)收集到的33pb^－1的Ψ(3770)数据,寻找D介子味道改变中性流(FCNC)和轻子数不守恒(LNV)的稀有衰变, 包括4个D⁰介子的衰变模式(K⁰e⁺e^－,Φe⁺e^－,ρ⁰e⁺e^－和K^*0e⁺e^－)和6个D⁺介子的衰变模式(K^－e⁺e⁺,K⁺e⁺e^－,π^－e⁺e⁺, π⁺e⁺e^－,K^*－e⁺e⁺和K^*+e⁺e^－). 没有发现信号,给出90%置信水平的上限. 其中, D⁺介子的两个衰变模式D⁺→K^*－e⁺e⁺和D⁺→K^*+e⁺e^－的上限是首次测量.     

在高能e+e－对撞机上探测top-Higgs的可能性

计算了top-Higgsh0t对过程e⁺e^－→tc νeνe,e⁺e^－→γ(Z)tc的贡献,并进一步讨论了在高能线性e⁺e^－对撞机(LC)上探测此粒子的可能性.结果表明:h0t对过程e⁺e^－→tc νeνe的贡献很大,通过此过程可在LC实验中探测top-Higgs;另外e⁺e^－→γtc也是探测h0t的有效过程.     

L3实验单W产生截面及反常耦合常数的测量

使用1996和1997年在L3探测器上获得的数据,对单W粒子产生过程e⁺e^－→e^－ν_eW⁺和e⁺e^－→e⁺νe W^－的反应截面做出了测量,并根据测量结果给出WWγ三玻色子耦合的反常耦合常数为:－0.65<△κ_γ,<0.82,－1.37<λ_γ<0.92.实验结果在误差范围内是与标准模型的理论值一致的,没有发现反常耦合常数存在的迹象.     

TC2理论在LC实验中的可能物理迹象

在高能e⁺e^－碰撞实验(LC)中，研究了顶色辅助的人工色(TC2)理论所预言的中性top介子 的产生. 结果表明，在LC实验中通过过程e⁺e^－→tc, e⁺e^－→γtc和e⁺e^－→Ztc可以探测到πt0的物理迹象.     

最小Higgs模型在ILC上可能的味改变物理迹象

在最小Higgs(LH)模型中, 由于引进了类矢量顶夸克T, 对弱作用流产生了新的影响. CKM矩阵从3×3变为4×3, 在树图下出现味改变中性流(FCNC). 本文研究了在国际高能直线对撞机(ILC)上能否通过e⁺e^－→tc+tc和e⁺e^－→WWν_eν_e→(tc+tc) ν_eν_e过程探测到LH模型所预言的FCNC信号.     

J/ψ强子衰变过程的角分布螺旋度形式

本文给出了e⁺e^－→J/ψ→V+X,V→P₁P₂和e⁺e^－→J/ψ→V+X,X→P₄P₅过程的角分布螺旋度形式.为e⁺e^－实验数据分析提供了理论公式.     

中性top-pion的产生和衰变

研究了顶色辅助的人工色(TC2?)理论预言的中性top-pion π0t的产生和衰变.结果表明:在高能正负电子对撞(LC)实验中,通过e⁺e^－→γπ0t和e⁺e^－→Z π0t过程可以产生大量的π0t粒子,通过e⁺e^－→γπ0t→γtc和e⁺e^－→π0tZ→tcZ过程可以探测中性top-pion π0t?的可能物理迹象.     

BeCl分子电子激发态的多参考组态相互作用计算

运用含Davidson修正的多参考组态相互作用方法,在aug-cc-pVTZ基组水平上,对BeCl分子基态和相同多重度的几个低电子激发态进行了势能扫描计算.通过群论原理确定各电子态对称性及离解极限.将其中基态(X²Σ⁺)和第一激发态(A²Π})对应的势能曲线拟合到Murrell-Sorbie解析势能函数形式,得到基态(X²Σ⁺)的离解能及主要光谱常数(括号中为文献[6]提供的实验值)为D_e=3.74eV,R_e=0.18173nm(0.17970),w_e=857.4cm¹(847.2),w_ex_e=5.03cm^-1(5.14),B_e=0.7103cm^-1(0.7285),α_e=0.0059cm^-1(0.0069),第一激发态(A²Π)的D_e=3.02eV,R_e=0.18369nm(0.18211),w_e=832.7cm^-1(822.1),w_ex_e=5.93cm^-1(5.24),B_e=0.6953cm^-1(0.7094),α_e=0.0065cm^-1(0.0068),计算结果与实验值符合得较好.另外,通过Level程序求解双原子径向核运动的Schrödinger方程得到J=0时BeCl分子这两个电子态的全部振动能级.     

高能正负电子对的湮没与超窄共振ψ粒子的作用

本文给出了R=(σ(e⁺e^-→强子))/(σ(e⁺e^-→μ⁺μ^-))随能量上涨的一个解释。研究了新发现ψ粒子所具有作用的性质,指出其强度f²/(4π)～10^-5—10^-6。求得峰值截面σ₀=(12π)/m_ψ²(Γ(ψ→e⁺e     

e+e－湮没中的胶子碎裂

本文假定e⁺e^－湮没时产生的胶子的强子化,胶子首先劈裂成一对等效的夸克、反夸克对.夸克之间的色相互作用,碎裂成末态强子.由此计算的e⁺e^－→3jet事例中的带电粒子多重数,胶子与夸克jet中多重数比率,以及e⁺e^－三胶子事例中的重子比率,都与实验结果一致.解释了e⁺e^－→3jet末态粒子的角分布.     

Absorption of dark matter by a supermassive black hole at the galactic center: Role of boundary conditions

The evolution of the dark matter distribution at the Galactic center is analyzed. It is caused by the combination of gravitational scattering by stars in the Galactic nucleus (bulge) and absorption by a supermassive black hole at the center of the bulge. Attention is focused on the boundary condition on the black hole. It is shown that its form depends on the energy of dark matter particles. The modified flux of dark matter particles onto the black hole is calculated. Estimates of the amount of absorbed dark matter show that the fraction of dark matter in the total mass of the black hole may be significant. The density of dark matter at the central part of the bulge is calculated. It is shown that recently observed γ radiation from the Galactic center can be attributed to the annihilation of dark matter with this density.     

演化过程主导的流体力学模型与Cu-Cu在BNL-RHIC能量碰撞中带电粒子的赝快度分布

高能重离子碰撞产生的带电粒子由两部分组成:一部分来源于碰撞产生的高温高密度物质,另一部分是带头粒子。假设高温高密度物质按照由演化过程主导的流体力学的规律膨胀并冻析为带电粒子,带头粒子来源于参与者且具有大致相同的能量。基于该假设,得到了高能重离子碰撞带电粒子的赝快度分布,并与BNL-RHIC上的PHOBOS合作组在sNN(1/2)=62.4与200 Ge V的Cu-Cu碰撞中给出的实验结果相比较,理论与实验测量符合得很好。     

Dark Matter

I review the development of the concept of dark matter. The dark matter story passed through several stages, from a minor observational puzzle to a major challenge for theory of elementary particles. Modern data suggest that dark matter is the dominant matter component in the Universe and that it consists of some unknown non-baryonic particles. Dark matter is the dominant matter component in the Universe; therefore, properties of dark matter particles determine the structure of the cosmic web.     

Evolution of the dark matter distribution at the galactic center

Annihilation radiation from neutralino dark matter at the Galactic center (GC) would be greatly enhanced if the dark matter were strongly clustered around the supermassive black hole (SBH). The existence of a dark matter "spike" is made plausible by the observed, steeply rising stellar density near the GC SBH. Here the time-dependent equations describing gravitational interaction of the dark matter with the stars are solved. Scattering of dark matter particles by stars would substantially lower the dark matter density near the GC SBH over 10 Gyr, due both to kinetic heating and to capture of dark matter particles by the SBH. This evolution implies a decrease by several orders of magnitude in the observable flux of annihilation products compared with models that associate a steep, dark matter spike with the SBH.     

Hidden supersymmetry

Inspired by the concept of complementarity, we present a illustrative model for the weak interactions with unbroken gauge symmetry and unbroken supersymmetry. The observable particles are bound states of some more fundamental particles. Supersymmetry is broken at the macroscopic scale of the observable particles by a discrete symmetry but remains exact at the scale of the fundamental particle and is thus hidden. This provides a link between theories at very high energies and the observed particle physics. Supersymmetric particles are confined in usual matter.     

Stable massive particles at colliders

We review the theoretical motivations and experimental status of searches for stable massive particles (SMPs) which could be sufficiently long-lived as to be directly detected at collider experiments. The discovery of such particles would address a number of important questions in modern physics including the origin and composition of dark matter in the universe and the unification of the fundamental forces. This review describes the techniques used in SMP-searches at collider experiments and the limits so far obtained on the production of SMPs which possess various colour, electric and magnetic charge quantum numbers. We also describe theoretical scenarios which predict SMPs along with the phenomenology needed to model their production at colliders and interactions with matter. In addition, the interplay between collider searches and open questions in cosmology such as dark matter composition is addressed.     

Constraints from the Wilkinson microwave anisotropy probe on decaying cold dark matter

We reformulate cosmological perturbations in the decaying cold dark matter model, and calculate cosmological microwave background anisotropies. By comparing our predictions with data from the Wilkinson Microwave Anisotropy Probe, we derive a new bound on the abundance and lifetime of decaying dark matter particles. The lifetime is constrained to Gamma(- 1)> or =123 Gyr at 68% C.L. (52 Gyr at 95.4% C.L.) when cold dark matter consists only of such decaying particles. We also consider a more general case and show that the constraint generalizes to Omega(DDM )h2 less, similar -0.5(Gamma (-1)/1 Gyr) (-1)+0.12 for Gamma(- 1)> or =5 Gyr at 95.4% C.L.     

暗物质及暗物质粒子探测

文章首先对暗物质的概念作了简单介绍,接着介绍了暗物质的发现过程和暗物质存在的证据等.随后,介绍了目前人们对暗物质粒子基本性质的理解和目前比较流行的暗物质模型,并解释了弱相互作用重粒子(WIMP)为什么获得人们最多的关注.文中还简单介绍了目前探测暗物质粒子的三种实验方法:对撞机探测法、直接探测法和间接探测法.最后,介绍了目前暗物质探测的最新进展,包括来自DAMA,CoGent,PAMELA,ATIC,Fermi等实验的最新结果.     

Direct detection constraints on superheavy dark matter

The dark matter in the Universe might be composed of superheavy particles (mass greater, similar 10(10) GeV). These particles can be detected via nuclear recoils produced in elastic scatterings from nuclei. We estimate the observable rate of strongly interacting supermassive particles (simpzillas) in direct dark matter search experiments. The simpzilla energy loss in Earth and in the experimental shields is taken into account. The most natural scenarios for simpzillas are ruled out based on recent EDELWEISS and CDMS results. The dark matter can be composed of superheavy particles only if these interact weakly with normal matter or if their mass is above 10(15) GeV.     

Narrowing the window for millicharged particles by CMB anisotropy

We calculate the cosmic microwave background (CMB) anisotropy spectrum in models with millicharged particles of electric charge q～10^?6?10^?1 in units of electron charge. We find that a large region of the parameter space for the millicharged particles exists where their effect on the CMB spectrum is similar to the effect of baryons. Using WMAP data on the CMB anisotropy and assuming the Big Bang nucleosynthesis value for the baryon abundance, we find that only a small fraction of cold dark matter, Ω_mcp<0.007 (at 95% CL), may consist of millicharged particles with the parameters (charge and mass) from this region. This bound significantly narrows the allowed range of the parameters of millicharged particles. In models without paraphotons, millicharged particles are now excluded as a dark matter candidate. We also speculate that recent observation of 511-keV γ rays from the Galactic bulge may be an indication that a (small) fraction of cold dark matter is comprised of millicharged particles.