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.     

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.     

暗物质粒子的质量与物态

讨论一类与宇宙超大尺度结构有关的、稳定的弱作用暗物质粒子,它们很可能是处在简并态的费米子(也可能处在近高温态)和处在近高温态的玻色子,其质量均为～10^－1eV,而其化学势的绝对值均远小于10^－1eV,这个结果与超高能原初宇宙线能谱在～10¹⁵eV及～10¹⁸eV附近出现拐折的现象不相矛盾.     

暗物质粒子属性和宇宙结构形成

暗物质是宇宙的主要物质成分,但其本质是什么仍然是现代科学亟待解决的一个重大问题。粒子物理学提供了多种暗物质粒子的候选者,不同的暗物质模型在宇宙小尺度结构方面有迥然不同的预言,所以原则上人们可以通过天文观测来限制暗物质粒子的属性。文章首先综述了暗物质粒子属性对宇宙结构形成的影响,然后阐述目前流行的冷暗物质宇宙学模型面临的一些困难,最后讨论用天文学区分冷、温暗物质模型的天文学方面研究进展情况。     

暗物质理论研究进展

评述了天体物理中暗物质的发现以及标准模型所面临的问题,综述了解决这些问题及标准模型之外可能出现的新物理与暗物质的联系。介绍了暗物质粒子选择条件和可能的暗物质粒子的候选者;对圆柱形暗物质表面密度与星系和星系团暗物质晕的晕核半径的关系进行了讨论,与其他模型进行了比较,得出暗物质晕的特征半径r_*的暗物质表面密度分布不是一个普适量;并叙述了近几年暗物质研究中提出的新理论模型-Hidden dark matter,最后叙述了中国暗物质实验探测研究的进展,2016年底DAMPE的第一批数据有可能给出;中国锦屏地下实验室（CJPL）的CDEX和PandaX合作组的第一期实验没有发现暗物质粒子存在的信号,期待他们下期的实验。A review of the evidence of the dark matter found in universe and the problems faced by the standard model. To address these issues as well as the possible relationship between the new physics beyond the standard model and dark matter, and given the selection condition of dark matter and possible candidates of the weakly-interacting massive particles (WIMPs). The correlation between the column surface density and the halo core radius of the dark matter halos of galaxies and cluster of galaxies is discussed, and the other models are compared. We find that the surface density within the halo characteristic radius r* is not an universal quantity; The new model (hidden dark matter)proposed in the study of dark matter is described. At last, the research progress of dark matter experiment in China is commented. At the end of 2016, the first batch of DAMPE data may be given;No significant excess events of WIMPS were found in the first stage of both the CDEX and PandaX experiments located in the China Jinping Underground Laboratory(CJPL). Look forward to their the next stage of these experiments in CJPL.     

基于DAMPE的暗物质间接探测研究进展

20世纪30年代天文学观测对标准宇宙模型提出了严峻挑战,为了调和观测数据与理论模型的矛盾,理论物理学家提出了暗物质理论;此后,实验物理学家据此摸索出了各种暗物质探测方案.本文将从暗物质概念的由来、暗物质基本性质、暗物质探测原理及方法和DAMPE在探测暗物质方面的最新进展几个方面展开介绍.重点以DAMPE的数据为基础,以电子谱分析为核心,在前人的研究基础上,对DAMPE数据和结果进行多层次、多方位的综合,进一步阐述了DAMPE电子谱中出现的TeV拐折和尖锐信号包含的深刻意义;最后依托研究过程中得到的一些信息,对未来暗物质探测实验提出一点看法和见解.     

反质子与原子核的非弹性碰撞

在扭曲波冲量近似的框架下,本文讨论了A(p,p)A非弹性碰撞.并具体地计算了能量为46.8MeV和179.7MeV的¹²C(p,p)¹²C的 2⁺,3^－态微分截面.用严格的分波法处理扭曲波.计算表明,反质子非弹性过程用DWIA是一个好的近似.同时,讨论了束缚态行为的重要性.由于反质子受核的强吸收原因,要求具有准确的核外束缚态波函数.     

中能区反质子与原子核的弹性散射

运用实验的pN散射振幅和多次散射理论,在冲量近似下考虑反质子能量从180MeV至1800MeV的光学势,发现此能区反质子光学势的虚部强度在130—140MeV附近.用所获得的光学势,计算¹²C,²⁶O,⁴⁰Ca和²⁰⁸Pb等满壳层核在五个能量下的弹性散射微分截面.看到所用的光学势,在180MeV能很好地符合实验数值.本文还预示了此能区在各个核上的理论结果.     

激光辅助的电子偶素对反质子的反氢生成反应

在一级玻恩近似下, 研究了在激光辅助的电子偶素-反质子碰撞中的反氢合成. 发现在小角范围内, 平行于电子偶素入射方向极化的激光使反氢生成截面变小. 在中等角度范围, 截面有一定的增加, 特别当偏振方向垂直于入射方向时, 截面增加比较明显.     

反质子物理

本文介绍反质子与核子和与原子核碰撞后各种物理现象．它与核子的散射获得的位势是吸引势和吸收型,与核的光学势是强吸收到．湮没后产生众多的介子和重子．以及在高能下湮没产生奇特性粒子、带粲的介子、重子．并探索获得混杂子、在核中存在反质子、其它新粒子的可能性． In this paper several physical phenomena of antiproton-nucleon and antiproton-necleus collision are discussed. The potential obtained from p-N scattering is attraction and absorption type. The optical potential of nucleus is strong absorption type. The annihilation happens after pp collision and thenproduces many kinds of meson, hadron, even produce some exotic particle and charmonium at high energy pp anihilation. Posibilities to find hybrids, antiproton and other particles in nucleus are also explored.     

Extending the MSSM with Singlet Higgs and Right Handed Neutrino for the Self-Interacting Dark Matter

In order to meet the requirement of BBN,the right handed neutrino is added to the singlet Higgs sector in the GNMSSM.The spectrum and Feynman rules are calculated.the dark matter pheonomenology is also studied.In case of λ ~ 0,the singlet sector can give perfect explanation of relic abundance of dark matter and small cosmological structure simulations.The BBN constraints on the light mediator can be easily solved by decaying to the right handed neutrino.When the λ_N is at the order of O(0.1),the mass of the mediator can be constrained to several MeV.     

理解暗能量和暗物质之间的相互作用

从热力学角度研究了暗能量和暗物质之间的相互作用. 假设相互作用是平衡态上的涨落并考虑此涨落导致的熵的修正, 导出了相互作用的物理表述, 把我们模型和观测结果作了比较.     

Large Number, Dark Matter, Dark Energy, and Superstructures in the Universe

Since there may exist dark matter particles ν and δ with mass - 10^-1 e V in the universe, the superstructures with a scale of 10^19 solar masses （large number A - 10^19） appeared during the era near and before the hydrogen recombination. Since there are superstructures in the universe, there may be no necessity for the existence of dark energy. For checking the superstructure in the universe by CMB anisotropy, we need to measure CMB angular power spectrum especially around ten degrees across the sky- in more details, While neutrino u is related to electroweak unification, the fourth stable elementary particle 6 may be related to strong-gravity unification, which suggests p ＋ p^- → n ＋ δ^- and that some new baryons appeared in the TeV region.     

Tachyonic Dark Matter

Recent attempts to explain the dark matter and energy content of the universe have involved some radical extensions of standard physics, including quintessence, phantom energy, additional space dimensions, and variations in the speed of light. In this paper I consider the possibility that some dark matter might be in the form of tachyons. I show that, subject to some reasonable assumptions, a tachyonic cosmological fluid would produce distinctive effects, such as a surge in quantum vacuum energy and particle creation, and a change in the conventional temperature–time relation for the normal cosmological material. Possible observational consequences are discussed.     

大数猜想与暗物质

讨论恒星质量、核子质量、暗物质粒子质量和普朗克质量四者间通过大数A～10¹⁹联系在一起,而且强相互作用与引力间也唯象地通过大数A似乎有着某种深层的联系.     

Restudy on Time-Evolution of SUSY Dark Matter

We restudy the Lee-Weinberg time-evolution equation including the R-parity violation. We carefullyanalyze the intluence of the boundary conditions, equation of state, SUSY parameters, especially the R-parity violation,and other factors on the time-evolution of the SUSY cold dark matter. Our numerical results show that without Rparity violation, only two ranges 20 ＜ mx01 ＜ 30 GeV and 75 ＜ mx01 ＜ 110 GeV can be consistent with data, if30 ＜ mx01 ＜ 75 GeV, there must be at least two kinds of heavy particles contributing to the cold dark matter. However,with the R-parity violation, the heavy neutralino can be dark matter constituent, but it must decay and the R-parityviolation parameter is constrained by the present data.