高速受电弓气动减阻的仿真优化研究

随着绿色环保的现代轨道交通设计理念发展,受电弓减阻成为制约高速列车提速的关键问题之一.高速列车运行时,受电弓暴露于流线型车体之外,是列车气动阻力的主要来源之一,随着列车速度的提高,受电弓的减阻问题亟待解决.本文针对某型高速受电弓,基于计算流体动力学仿真技术,分析了整弓气动阻力分布,确定滑板与底座的压差阻力是气动阻力的主...     

关于参数型copula函数的拟合检验

在金融和保险中,copula函数是一种构造多元相关分布函数的有力工具．然而,怎样选择一个适当的copula函数用于拟合数据,并没有找到统一的方法．因此,基于copula函数的经验分布,我们提出了一种用于检验具有某种特定参数结构的copula函数拟合数据优良性的方法,并得到了此检验的渐近性质．由于该检验统计量的极限分布依赖未知参数,我们采用非参数蒙特卡罗方法确定临界值．我们做了一个简单的模拟来验证本文提出的检验方法的功效．     

Bose-Einstein Condensates in a One-Dimensional Optical Lattice: from Superfluidity to Number-Squeezed States

We study the phase coherence property of Bose-Einstein condensates confined in a one-dimensional optical lattice formed by a standing-wave laser field. The lattice depth is determined using a method of Kapitza-Dirac scattering between a condensate and a short pulse lattice potential. Condensates are then adiabatically loaded into the optical lattice. The phase coherence property of the confined condensates is reflected by the interference patterns of the expanded atomic cloud released from the optical lattice. For weak lattice, nearly all of the atoms stay in a superfluid state. However, as the lattice depth is increased, the phase coherence of the whole condensate sample is gradually lost, which confirms that the sub-condensates in each lattice well have evolved into number-squeezed states.     

Statistical analysis of Fe abundances gradients in the Galaxy

Using the high precision data of the proper motions and parallaxes from Hipparcos catalogue, we obtained the orbital parameters of 1302 stars in the Galaxy based on the mass distribution model provided by Allen and Santillón. Fe abundances of 1295 stars among our samples were analyzed. With the correlation analyses between [Fe/H] and orbital parameters, we obtained that the Fe gradient is - 0.057 ± 0.007 dex/kpc along the direction of the maximum galactocentric distance (hereafter DG_max) in the range of 8.5 kpc < DG_max < 17 kpc. We also got the result that the vertical gradient is steeper than the radial gradient. Furthermore, we divided the samples into two subgroups: giants and dwarfs; F, G and K stars; and then analyzed them respectively. Our results show that the gradient becomes flatter and flatter from giants to dwarfs, from F type to G and K type stars. We also divided the samples into disk and halo stars using maximum vertical distance Z_max = 1 kpc as the criterion and got the result that the abundances of the disk stars are much higher than that of the halo stars. Our work suggests the existence of the galactic gradient and supports those chemlcal evolution medels which show that the halo was formed before the disk at the early stage of the Galaxy.     

中学生如何建立自己合理的物理知识结构?

 在积累知识的过程中,除如何猎取知识外,还有一个如何储存知识的问题.深刻的理解加上合理的储存,就能运用自如地掌握知识,而靠死记硬背储存知识,遇到灵活性强、比较隐蔽的问题就束手无策了.合理的知识结构应当具有以下特征:一、系统性.处于游离状态的知识,完全失去了其应有价值,成了大脑的负担;而系统化的知识,各个知识点前后呼应,表现出1+1>2的价值,减少了记忆量和记忆难度.因此,学习中不仅要善于获得知识,更要善于整理自己的知识系统.     

基于主Hessian方向的中央均值子空间边际坐标检验

本文给出了基于两种相近的主Hessian方向方法的边际坐标检验. 这种检验方法能够非常有效的识别自变量对于回归均值中央子空间的贡献. 此外, 与利用切片逆回归和切片平均方差估计的检验方法不同的是, 本文中主Hessian方向的检验方法可以避免对切片数目的选择. 我们证明了检验统计量在原假设下的渐近分布, 并且通过模拟, 证实了检验的有效性.     

基于真实数据的天文教学实践探索

介绍在利用斯隆数字巡天数据进行宇宙探索的教学和研究案例的基础上,以真实数据平台万维天文望远镜为例,描述华中师范大学天文学类课程基于真实数据的天文教学实践探索,主要从WWT平台提供良好的资源环境、是良好的信息加工工具、是良好的研发平台3个方面予以陈述.     

基于纳米压痕的氧化镓晶体断裂韧度检测方法研究

为了快捷、精准测量脆性易解理氧化镓晶体的断裂韧度,为氧化镓精密加工提供理论依据.采用G200纳米压痕仪对氧化镓晶体进行纳米压痕试验,通过扫描电子显微镜分析压痕形貌,分别采用纳米压痕法、能量法两种方法计算断裂韧度.纳米压痕法测得(010)面氧化镓晶体的断裂韧度为0.769 MPa·m1/2;能量法测得其断裂韧度为0.782 MPa·m1/2.与传统的断裂韧度检测方法相比,基于纳米压痕仪的压痕法和能量法能够微损伤快速检测脆性材料的断裂韧度.能量法是更精准、更便捷的纳米级断裂韧度检测方法.     

镜煤吡啶不溶物及其热解加氢产物的NMR研究

本文对镜煤吡啶不溶物、热解加氢后吡啶及四氢呋喃不溶物进行了固体NMR研究,获得了12种结构参数,并对热解加氢产物中的苯可溶各馏份进行了一维、二维液体NMR研究,归属了其¹³C和¹H谱,计算了各馏份的平均分子结构.     

Abundance gradients in the galactic disk

The relationship between abundances and orbital parameters for 235 F- and G-type intermediate- and low- mass stars in the Galaxy is analyzed. We foundthat there are abundance gradients in the thin disk in both radial and verticaldirections (-0.116 dex kpc-1 and -0.309 dex kpc-1 respectively). The gradients appear to be flatter as the Galaxy evolves. No gradient is found in the thick disk based on 18 thick disk stars. These results indicate that the ELS model is mainly suitable for the evolution of the thin disk, while the SZ model is more suitable for the evolution of the thick disk. Additionally, these results indicate that in-fall and out-flow processes play important roles in the chemical evolution of the Galaxy.