InC_n~+和InC_n~-(n=1～10)团簇的结构和性质比较研究

利用密度泛函理论对碳基混合团簇InC_n~+和InC_n~-(n=1～10)的结构和性质进行了比较研究,结果表明,除了InC_2~+/InC_2~-团簇(最稳定构型为等腰三角形)外,这两类型团簇的最稳定结构都是In原子位于碳链一端的直线型或准直线型。阳离子团簇InC_n~+是n为偶数的团簇基态是三重态,n为奇数的团簇基态是单态,而阴离子团簇InC_n~-是n为偶数的团簇基态是单态,n为奇数的团簇基态是三重态,刚好与阳离子团簇相反。增量结合能和能量二阶差分的比较分析得出:这两种团簇的稳定性都随尺寸的增加展现出强烈的奇偶振荡特性,阳离子团簇的稳定性是奇强偶弱;而阴离子的情况刚好相反。电离能IP_(ad)和亲和势EA_(ad)的计算结果也展示出相同的振荡规律。阳离子团簇的磁矩表现出强烈的奇强偶弱的振荡规律,但阴离子团簇的振荡规律刚好相反。两种团簇基态结构的极化率张量的平均值及各向异性不变量都呈现出增大的趋势。     

LN9015—1 ISO配合飞机结构的配合选择

IV HI l _口二n 回*6-u8 Sbcub“‘.*bZ nbib“J *垄里I pb)互7 尸片d92 C]】回Hy【H丛“’SH]回]卜u“罗 Hrtthth’1. 111 巨十34D 十20 十卫0 十 Hs n D 0 D n D一91 一 8D 一下屋D 一20 D 一 Rm个且0 小问刑D+Rn 牛2q 68十川N 十]dJ +dl nJ“3_]川_Bn2_黑1_可CZ_*q]dC【JQm ng n D n 个曹互 >8D卡州D 十27 十]61十gDnDnlnl.血1.下n【_9nD.znl 一7M个】川 十曹烫【小*【D 十二n ;- hi十2月J J 十]91 十 且j+曹]凤3 回印7F1_1刊 一991_*p【.6nl—IARIngnDnl+*n >bl个5o 十zZ 十lq 十11SIBllll Cl—12l_9F7 州 一 O1…     

风车不平衡模拟碰摩实验台动力学特性研究

针对民用大涵道比涡扇发动机风车不平衡振动问题,搭建了转子-轴承-机匣系统风车不平衡模拟碰摩实验台,建立了转子实验台的简化有限元模型,并通过实验测得临界转速验证了模型的有效性。碰摩实验前,数值仿真分析了风车不平衡状态下不同碰摩刚度和碰摩间隙对转静碰摩系统动力学响应的影响,对碰摩实验结果进行了预估判断。结果表明:在低转速大不平衡量的风车不平衡模拟条件下,碰摩刚度的变化会激发n/2(n=1,5,7)倍频及4倍频的转频分量;碰摩间隙的变化除激发n/2(n=1,5)倍频的转频分量外,也会激发n/5(n=3,11,13,21)倍频的转频分量。     

相关系数ARMA(p,q)序列分析方法

本文提出相关系数ARMA(p,q)序列分析方法。相关系数ARMA(p,q)序列是从非平稳序列中分离出的一类工程上常见且便于研究的时间序列,在模式识别、故障诊断、信号处理、自动控制和结构响应分析等领域有着广泛的应用。传统的相关函数ARMA(p,q)序列仅是它的一个特例。文中建立了相关系数ARMA(p,q)序列的条件极大似然估计和精确极大似然估计,前者在样本较大时简单便于工程应用,后者则在样本较小时仍具有较高的精度,它们通过时域的全程分析,充分利用样本信息确定相关系数ARMA(p,q)序列的均值函数、方差函数和相关系数函数。在此基础上可进行高精度的频谱分析。     

电磁方法在铸造中的应用(五)—镁合金的工频熔化电磁搅拌电磁输送 第三篇 电磁输送(下)

搜鸳一也台另巨二二角丽电磁输送二(六)平面电磁泵的设计计算实例 1.给定条件 1)输送材料:ZM一5合金液 2)液态比重:Y=1.5克/厘米只 3)电阻系数:p(700℃以上)=31 X 10一6 欧姆一厘米 4)输送工作温度t=750℃左右 5)流量:Q二3.0公斤/秒 6)压力么p二0.4公斤/厘米z 7)f=50赫芝 2.确定电磁泵的基本参数 1):二37 .5厘米 Zc=20厘米 2)P=1 3)q=33.计算 1)V:二Zrf=2丫37.5冰50=3750厘米/秒 2)V、=Q/F、 F、一泵沟截面积 Fl,=a xZb 取Zb二260毫米 a二15毫米 Fl、二Zb Xa=39厘米匕 Q=3.0公斤/秒二2000厘米吕/秒200039 .0二51.3厘米/秒3)S4)1Vf…     

高Q腔法测试透波材料毫米波复介电常数

介绍了透波材料毫米波复介电常数自动测试方法,采用高Q腔一腔多模扫频(18～40 GHz)方法测试了微波低损耗圆盘状介质材料,谐振腔工作在TE10p模式,电场的极化方向平行于样品表面.为适应毫米波段材料测试的要求,在设计测试用宽频高Q值谐振腔时,改变以往工作中腔壁开槽位置以抑制TM1mn简并模,对测试用谐振腔的设计大大减小了测试误差.用此系统对几种低损耗材料进行测量,结果证明谐振腔有效Ё抑制了干扰模式,减小了测试误差.对测试结果进行了误差分析,系统的最可几测试误差为:|△εr/εr|=2%;|△tanδ|=10%tanδ+5×10-5.     

飞控系统余度信号奇异故障处理策略研究

飞机机翼、操纵面的对称性设计,决定了飞控系统传感器、计算机和舵机等部件在飞机上分布式对称安装并选择偶数n 余度的体系架构。余度部件生产关系的平衡分工,不同厂家设计、制造的差异,不可避免地出现“两派对立”的偶数分离和“互不认可”的奇异故障。本文提出了中位数表决、变化量记忆、余度重构等基础理论,给出了极端信号大概率故障判据,研究论证了这些基础理论和判据的科学原理。为四余度信号“2∶2 不确定故障、1∶1∶1∶1 多故障”、三余度信号1∶1∶1 多故障和二余度信号1∶1 故障,提供了有效的表决监控方案。     

相关系数平稳序列的估计与识别

本文提出了通过观测序列确定不可直接测得的相关系数平稳序列模型参数的方法,详细讨论了相关系数AR(p),MA(q)和ARMA(p,q)序列状态方程的参数估计,为非平稳序列的滤波、预测和平滑提供了依据。文中还给出了观测系统参数的识别方法,与传统方法相比,本文方法考虑了测量噪声的均值和方差随时间变化情况,具有更高的识别精度。      

硝酸根与柠檬酸的摩尔比对低温燃烧合成钛酸钡的影响

以Ba(NO3)2-TiO2-C6H7O8@H2O为体系,在600℃的加热温度下进行低温燃烧合成实验,制得粒度为200n～350nm的四方相BaTiO3陶瓷粉体.研究表明体系中硝酸根与柠檬酸的摩尔比为2.5～3.0时,体系燃烧最完全,形成比表面高(2.47m2/g)、颗粒细小、孔隙率大的钛酸钡粉末.     

有限局部环上酉群的Sylow子群

设K=Fq2,其特征为p,q=pα,K有对合自同构:ωa|→aq,G是一个p-群,其阶为p,β群代数R=KG为一局部环。本文给出了R=KG上酉群U2nR的Sylow子群,若charK=p,U2nR的Sylow p-子群同构于某些特殊形式的矩阵生成的子群;若charK=p≠l,U2nR的Sylow l-子群同构于一循环群或半二面体群与若干Zl型循环群的圈积。     

False alarm analysis of the envelope detection GO-CFAR processor

The greatest of constant false alarm rate processor (GO CFAR) is a useful architecture for adaptively setting a radar detection threshold in the presence of clutter edges. The GO CFAR input is often the envelope detected in-phase (I) and quadrature (Q) channels of the baseband signal (x_e=√(I²+Q²)). This envelope detection can also be approximated using x=a max{|I|,|Q|}+b min{|I|,|Q|} which requires less complex hardware (a and b are simple multiplying coefficients). The envelope GO CFAR processor and several envelope approximation GO CFAR processors are compared in terms of the probability of false alarm (PFA) performance. Closed-form expressions which describe the PFA performance are given and their accuracy evaluated. It is shown that for all cases, the PFA is proportional to the number of reference cells n for small threshold multiplier T and inversely proportional to n for large T. A region of intersection occurs where the PFA is the same for two different values of n. For example, at T'=1.68 in the |I|+|Q| GO CFAR (a=1, b=1) the PFA for n=1 is equal to the optimal n=∞ fixed-threshold PFA (PFA=0.112)     

Theoretical modelling of Algol disks

A brief review of various theoretical approaches to model accretion disks is presented. Emphasis is given to models that determine self-consistently the structure of a disk together with the radiation field. It is argued that a proper treatment of the vertical structure is essential for calculating theoretical spectra to be compared with observations. In particular, it is shown that hot layers above an accretion disk (sometimes called disk chromospheres or coronae), whose presence is indicated by recent UV observations of strong emission lines of highly ionized species, may be explained using simple energy balance arguments.1987–88 JILA Visiting Fellow.This work was in part supported by a NASA grant ADP U-003-88 (Plavec and Hubeny). I also wish to thank the organizers of the IAU Colloquium 107 for the travel grant which enabled me to attend the meeting.     

Spectral Analysis with Sinusoids and Walsh Functions

The Walsh spectrum of a sinusoid of frequency f = p/2q with p odd consists entirely of lines at orders s that are odd multiples of 2/2q, and the Fourier spectrum of a Walsh function of order 2p/2q consists entirely of lines at frequencies that are odd multiples of 1/2q. For all other frequencies or orders, the spectrum contains no lines, but the power spectral density takes all values in the range [0,oo] in every interval, however short, while being almost everywhere zero. For detecting the presence of a sinusoid by means of Walsh analysis, the time scale should therefore be chosen so that the order of the Walsh function is a power of 2 and the Walsh function is a Rademacher function, i.e., a hard-limited sinusoid of the frequency being sought.     

二分图中哈密顿[k,k+1]因子

主要研究了在均衡二分图G中哈密顿[k,k 1]因子的存在性.设G=(X,Y,E),|X|=1Y1=2/n≥4(k-2)-3,k≥2且n≥2,δ(G)≥k,若G中每一对不相邻的顶点u,v有max{dG(x),dG(x)}≥4/n 2,则G有包含哈密顿圈C的[k,k 1]因子.在此基础上,进一步给出结论:二分图G=(X、Y、E),|x|=|Y|=2/n≥4(k-2)且n≥2,δ(G)≥k,若G中每一对不相邻的顶点u,v有dG(v)≥2/n 4,则G有包含哈密顿圈C的[k,k 1]因子.结论在很大程度上改进了已有的包含哈密顿圈的度条件,进一步完善了包含哈密顿圈的因子理论.     

The solar flare plasma: Observation and interpretation

In the past several years, X-ray observations of the Sun made from rockets and satellites have demonstrated the existence of high temperature (20 × 10⁶ – 100 × 10⁶ K), low density plasmas associated with solar flare phenomena. In the hard X-ray range ( < 1 ), spectra of the flaring plasma have been obtained using proportional and scintillation counter detectors. It is possible from these data to determine the evolution of the hard X-ray flare spectrum as the burst progresses; and by assuming either a non-thermal or thermal (Maxwellian) electron distribution function, characteristic plasma parameters such as emission measure and temperature (for a thermal interpretation) can be determined. Thermal interpretations of hard X-ray data require temperatures of 100 × 10⁶ K.In contrast, the soft X-ray flare spectrum (1 <<30 ) exhibits line emission from hydrogen-like and helium-like ions, e.g. Ne, Mg, Al, Si,... Fe, that indicates electron energies more characteristic of temperatures of 20 × 10⁶ K. Furthermore, line intensity ratios obtained during the course of an event show that the flare plasma can only be described satisfactorily by assuming a source composed of several different temperature regions; and that the emission measures and temperatures of these regions appear to change as the flare evolves. Temperatures are determined from line ratios of hydrogen-like to helium-like ions for a number of different elements, e.g., S, Si, and Mg, and from the slope of the X-ray continuum which is assumed to be due to free-free and free-bound emission. There is no obvious indication in soft X-ray flare spectra of non-thermal processes, although accurate continuum measurements are difficult with the data obtained to date because of higher order diffraction effects due to the use of crystal spectrometers.Soft X-ray flare spectra also show satellite lines of the hydrogen-like and helium-like ions, notably the 1s ²2s ² S-1s2s2p ² P transition of the lithium-like ion, and support the contention that in low density plasmas these lines are formed by dielectronic recombination to the helium-like ion. Also, series of allowed transitions of hydrogen-like and helium-like ions are strong, e.g., the Lyman series of S up to Lyman-, and ratios of the higher member lines to the Lyman- line can be compared with theoretical calculations of the relative line strengths obtained by assuming various processes of line formation.This review will discuss the X-ray spectrum of solar flares from 250 keV to 0.4 keV, but will be primarily concerned with the soft X-ray spectrum and the interpretation of emission lines and continuum features that lie in this spectral range.     

Physical mechanisms for turbulent dissipation in collisionless shock waves

Temporal and spectral characteristics of solar hard X-ray bursts are briefly reviewed. The merits of non-thermal and thermal flare models are discussed. The validity of these models may be checked by future measurements of X-ray polarization. Finally, some important results of recent satellite experiments are described providing information on the spatial distribution of hard X-ray sources: the multi-spacecraft observation of X-ray bursts and the imaging of X-ray sources by means of the HXIS instrument.Paper presented at the IX-th Lindau Workshop The Source Region of the Solar Wind.     

The Inner Heliosphere - Outer Heliosphere Comparison for Cosmic Ray Modulation

This paper summarizes cosmic ray data on both galactic and anomalous particles in the inner and outer heliosphere near the sunspot minimum in 1995 and 1996 at the end of solar cycle 22. These data come from the IMP spacecraft in the inner heliosphere and the Voyager and Pioneer spacecraft in the outer heliosphere. In the inner heliosphere, the cosmic ray intensities at all energies in 1996 have recovered to almost the same maximum values they had at the last sunspot minimum in 1987 and the intensities are an even closer match to those observed two 11-year cycles earlier in 1976. In the outer heliosphere beyond 40 AU the intensity recovery is very slow and the intensities at all energies and for all species are almost constant in 1995-96 indicating that little further recovery can be expected in this cycle. The intensity of galactic cosmic rays in 1996 is only 0.3-0.5 of that observed at the same radius of 42 AU in 1987 and for anomalous cosmic rays this ratio is only 0.1-0.2. This suggests a dramatically different entry of particles into the heliosphere in the two cycles for both types of particles as well as significantly different particle flow characteristics in the outer heliosphere. The net result of these different characteristics is that near the Earth only a relatively small intensity difference is observed between successive 11-year solar cycles whereas in the outer heliosphere the differences between cycles become very large and may even dominate the overall modulation.     

涡轮叶片尾缘出流对带叉排扰流柱阵列的内冷通道传热特性的影响

本文用实验的方法模拟研究了涡轮叶片尾缘出流对带叉排扰流柱阵列的内冷通道的对流换热特性的影响。实验模型通道为矩形通道,扰流柱的排列参数S_n/d为6.5,S_p/S_n为1.2,其中d为扰流柱的直径,S_n为扰流柱横向间距,S_p为2倍的纵向间距。矩形模型通道的长边与转轴的夹角为20°。研究了出流孔总面积A₀与通道最大截面积A的比值,雷诺数Re,转动数R₀等参数对传热特性的影响。并比较了尾缘出流与叶尖出流的换热特性。      

Implications of a weak termination shock

Recent observations from the Voyager spacecraft have suggested that the spectrum of the anomalous cosmic ray component is relatively steep at the termination shock, which is believed to be responsible for accelerating these particles. This conclusion argues that the termination shock must be weak, which in turn requires that the upstream Mach number in the solar wind must be quite low, 2.4. It is pointed out that such conditions are unlikely to prevail at all locations along the shock front. However, it is possible for such conditions to exist at the interface between high speed streams at high heliographic latitudes and the region at low latitudes where high and low speed streams have interacted and come into equilibrium. This discussion suggests a preferred location for the injection of the anomalous component into the shock acceleration process.     

循环对称结构特征值问题的复数域子空间迭代法

提出求解在循环对称结构固有特性问题的研究中出现的复Ｈｅｒｍｉｔｅ阵特征值问题的复数域子空间迭代法。根据Ｔｈｏｍａｓ等人提出的理论，生成循环对称结构任一子结构的复约束质量阵和复约束刚度阵。根据本文提出的办法，生成一个包含ｑ个相互质量正交归一的复向量组成的初始里兹迭代复向量组，并将原广义特征值问题的求解空间投影到由这ｑ个复向量张成的Ｋｒｙｌｏｖ空间上可很方便地在ｑ维Ｋｒｙｌｏｖ空间上进行广义复Ｈｅｒｍｉｔｅ矩阵特征值问题的求解。