室温熔盐二(三氟甲基磺酸酰)亚胺锂-尿素体系的分子动力学模拟

应用分子动力学模拟了25 ℃和50 ℃时新型室温熔盐二(三氟甲基磺酸酰)亚胺锂[LiN(SO2CF3)2, LiTFSI]与尿素(摩尔比为1:3.6)体系的结构与动力学性质. 在两个温度下体系的微观结构基本相同, Li+的配位数约为5, 且都是与溶剂和阴离子中的氧原子发生配位. 对TFSI-的研究表明, 每个TFSI-只提供四个氧中的一个与Li+配位; 而且在Li+的配位层中, TFSI-具有顺、反和gauche 等不同的构象, 并且不同构象出现的几率会随着温度的改变而改变.     

Multi-wavelength study of MGRO J2019+37

MGRO J2019+37,within the Cygnus region,is a bright extended source revealed by Milagro at 12-35 TeV.This source is almost as bright as the Crab Nebula in the northern sky,but is not confirmed by ARGO-YBJ around the TeV scale.Up to now,no obvious counterpart at low energy wavelengths has been found.Hence,MGRO J2019+37 is a rather mysterious object and its VHEγ-ray emission mechanism is worth investigating.In this paper,a brief summary of the multi-wavelength observations from radio toγ-rays is presented.All the available data from XMM-Newton and INTEGRAL at X-ray,and Fermi-LAT atγ-ray bands,are used to get constraints on its emission flux at low energy wavelengths.Then,its possible counterparts and the VHE emission mechanism are discussed.     

Geometry and optics calibration of WFCTA prototype telescopes using star light

The Large High Altitude Air Shower Observatory (LHAASO) project is proposed to study high energy gamma ray astronomy (40 GeV--1 PeV) and cosmic ray physics (20 TeV--1 EeV). The wide field of view Cherenkov telescope array, as a component of the LHAASO project, will be used to study the energy spectrum and composition of cosmic rays by measuring the total Cherenkov light generated by air showers and the shower maximum depth. Two prototype telescopes have been in operation since 2008. The pointing accuracy of each telescope is crucial for the direction reconstruction of the primary particles. On the other hand, the primary energy reconstruction relies on the shape of the Cherenkov image on the camera and the unrecorded photons due to the imperfect connections between the photomultiplier tubes. UV bright stars are used as point-like objects to calibrate the pointing and to study the optical properties of the camera, the spot size and the fractions of unrecorded photons in the insensitive areas of the camera.     

西藏羊八井广延空气簇射阵列性能的Monte Carlo研究

本文用Monte Carlo方法研究西藏羊八井空气簇射阵列性能.确定好事例判选标准.簇射中心定位精度达3.4m.原初粒子到达方向角分辨率好于1.1°.原初粒子能量按lgE₀=lg(0.45ΣN_i)±0.226确定,其中E₀(TeV)为初级入射粒子能量,ΣN_i为FT探测器上探测到的粒子总数.     

在羊八井测量初级宇宙线直达质子研究质子和空气核非弹性作用截面

提出了一种在高海拔通过测量直达质子来确定质子和空气核(p-air)的非弹性作用截面的方法, 并通过Monte Carlo模拟, 研究了其可行性. 假定将一台类似于KASCADE的强子量能器设置在西藏羊八井ARGO探测器的中央,选择大气簇射(AS)轴心落在强子量能器内的事例, 用全覆盖ARGO阵列作AS的反符合,用强子量能器测量非伴随的高能强子,即能以已知的效率得到一个直达质子事例样本. 利用这个样本,本工作以1%—2%的精确度还原了Monte Carlo模拟中所使用的p-air非弹性作用截面, 从而证明了这一方法的可行性.     

超高能中微子天文学实验现状

 中微子在粒子物理的标准模型中是一组很特殊的粒子，它们质量最轻（在标准模型中没有质量）因而几乎不受引力影响，不带电荷因而不受电磁相互作用的影响，只参与弱相互作用，但其寿命几乎是无穷长。如果中微子产生于遥远的高能天体，在到达地球的漫长传播过程中其路径不会被遍布宇宙的磁场所改变。中微子的这些特性使它与光子一起成为绝佳的天文学信息传播者，成为正在崛起的新兴中微子天文学学科发展的强劲原动力。与传统的光子天文学相比，中微子具有更加优越的特性，即不会与弥漫全宇宙的3K宇宙学背景光子发生作用，从而能够打开高于光子天文学所能工作的能量区域的观测窗口，譬如在高于10¹⁵电子伏特（记为PeV）的“超高能”区，探测中微子成为唯一的天文观测手段。 …………     

超高能软强子作用的Chou－Yang模型

用Ｃｈｏｕ－Ｙａｎｇ模型构造了一个用于＝２６ＧｅＶ到２２ＴｅＶ的软强子非单衍相互作用ＭｏｎｔｅＣａｒｌｏ产生器．结合大横动量喷注产生过程的ｐＱＣＤ计算和相应的部分子强子化方案，较好地再现了高能区实验的结果．平滑地外推到超高能区，预言了非弹性度随能量下降的趋势．     

超高能软强子作用的Chou–Yang模型

用Chou-Yang模型构造了一个用于s=26GeV到22TeV的软强子非单衍相互作用MonteCarlo产生器.结合大横动量喷注产生过程的pQCD计算和相应的部分子强子化方案,较好地再现了高能区实验的结果.平滑地外推到超高能区,预言了非弹性度随能量下降的趋势.     

分子动力学模拟离子液体（BMIM＋／PF6-）／金红石（110）界面的结构

本文用分子动力学方法研究了室温离子液体1-甲基-3-丁基咪唑六氟化磷（BMIM＋／PF6-）在金红石（110）晶面的结构性质,旨在模拟染料敏化太阳能电池中的电解液／半导体界面性质．模拟结果表明离子液体的密度函数在界面处出现最大值,并成有序的“双层”结构排列,在金红石表面区域,阳离子（BMIM＋）的侧链有明显伸长的趋势,且咪唑环倾向平行于金红石（110）晶面．     

A future project at tibet： the large high altitude air shower observatory （LHAASO）

Gamma ray source detection above 30 TeV is an encouraging approach for finding galactic cosmic ray sources. All sky survey for gamma ray sources using wide field of view detector is essential for population accumulation for various types of sources above 100 GeV. In order to target those goals, a large air shower particle detector array of 1 km^2 （the LHAASO project） at 4300 m a.s.l, is proposed, By adding two MagicⅡ- type telescopes in the array as proposed, LHAASO will be enhanced in source morphologic investigation power. The proposed array will be utilized also for energy spectrum measurement for individual cosmic ray species above 30 TeV. By re-configuring the wide field of view telescopes into fluorescence light detector array, the aperture of the detector array can be enlarged to cover an energy region above 100 PeV where the second knee is located. Cosmic ray spectrum and composition will be measured in order to transfer an energy scale to ultra high energy cosmic ray experiments.