相变光盘多层膜系结构的最佳光匹配研究

论述了相变光盘最佳膜系结构的设计。采用导纳矩阵法计算膜系的能量反射率，用量优化计算方法编程计算，提出了第二大极值解作为在工艺上可行的实用光盘的膜系结构，并按这种膜系结构制作样品，其擦写循环数达１００万次上。     

Halo White Dwarfs and Baryonic Dark Matter

We describe the formation of hot intergalactic gas along with baryonic remnants in galaxy halos. In this scenario, the mass and metallicity of the hot intracluster and intragroup gas relates directly to the production of baryonic remnants during the collapse of galactic halos. We construct a schematic but self-consistent model in which early bursts of star formation lead to a large remnant population in the halo, and to the outflow of stellar ejecta into the halo and ultimately the Local Group. We consider local as well as high redshift constraints on this scenario. This study suggests that the microlensing objects in the Galactic halo may predominantly be 0.5M white dwarfs, assuming that the initial mass function for early star formation favored the formation of intermediate mass stars with m 1M. However, the bulk of the baryonic dark matter in this scenario is associated with the ejecta of the white dwarf progenitors, and resides in the hot intergalactic medium.     

MP＊中的等值完全析取范式

讨论中介逻辑命题演算扩张系统ＭＰ＊中在等值意义下的完全析取范式的存在性和唯一性。引入ＭＰ＊中等值全板范式的概念，并用分步构造法证明这种范式在等值意义下是存在的，且是唯一的。     

运输环境中某战术导弹结构振动特性分析

应用三维有限单元和导弹实体简化模型对一种战术导弹的结构振动特性进行分析，并动用ＡＮＳＹＳ有限元分析程序，计算得到了“自由－固支”条件下，导弹竖立状态的固有模态，取得了与试验和数据基本一致的结果，证明了所建模型物正确性，进而对运输环境中导弹水平支承条件下的固有频率和振型进行了分析计算，所得结果为导弹的使用可靠性分析提供了依据。     

Solar Sources of Heliospheric Energetic Electron Events—Shocks or Flares?

Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks driven by coronal mass ejections (CMEs) with speeds ≳1000 km s⁻¹. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known several decades ago, but recent observations have presented a more complex picture. We review early and recent observational results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events; electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares. Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions for future work are given.     

Particle Acceleration Mechanisms

In this paper we review the possible mechanisms for production of non-thermal electrons which are responsible for the observed non-thermal radiation in clusters of galaxies. Our primary focus is on non-thermal Bremsstrahlung and inverse Compton scattering, that produce hard X-ray emission. We first give a brief review of acceleration mechanisms and point out that in most astrophysical situations, and in particular for the intracluster medium, shocks, turbulence and plasma waves play a crucial role. We also outline how the effects of the turbulence can be accounted for. Using a generic model for turbulence and acceleration, we then consider two scenarios for production of non-thermal radiation. The first is motivated by the possibility that hard X-ray emission is due to non-thermal Bremsstrahlung by nonrelativistic particles and attempts to produce non-thermal tails by accelerating the electrons from the background plasma with an initial Maxwellian distribution. For acceleration rates smaller than the Coulomb energy loss rate, the effect of energising the plasma is to primarily heat the plasma with little sign of a distinct non-thermal tail. Such tails are discernible only for acceleration rates comparable or larger than the Coulomb loss rate. However, these tails are accompanied by significant heating and they are present for a short time of <10⁶ years, which is also the time that the tail will be thermalised. A longer period of acceleration at such rates will result in a runaway situation with most particles being accelerated to very high energies. These more exact treatments confirm the difficulty with this model, first pointed out by Petrosian (Astrophys. J. 557:560, 2001). Such non-thermal tails, even if possible, can only explain the hard X-ray but not the radio emission which needs GeV or higher energy electrons. For these and for production of hard X-rays by the inverse Compton model, we need the second scenario where there is injection and subsequent acceleration of relativistic electrons. It is shown that a steady state situation, for example arising from secondary electrons produced from cosmic ray proton scattering by background protons, will most likely lead to flatter than required electron spectra or it requires a short escape time of the electrons from the cluster. An episodic injection of relativistic electrons, presumably from galaxies or AGN, and/or episodic generation of turbulence and shocks by mergers can result in an electron spectrum consistent with observations but for only a short period of less than one billion years.     

现代远程教育的媒体素材构建方法

本文阐述了媒体素材的采集及处理方法 ,对现代远程教育工程建设可提供有效的帮助     

基于概率的航空发动机飞行换算率改进算法

针对斯贝MK202发动机应力标准对零部件工作寿命评定中未包含各种随机因素的影响,考虑零部件疲劳性能参数的分散性和发动机整机载荷谱的随机性,将实测数据统计分析、零部件应力有限元分析以及蒙特卡罗模拟分析有机结合,提出了基于概率的航空发动机飞行换算率改进算法,以解释航空发动机零部件实际工作寿命存在的差异.经范例验证表明:确定性寿命评定方法的飞行换算率计算结果与改进算法下的平均值相当;对于单次飞行换算率,改进算法的单次飞行换算率平均值比确定性方法的计算结果小2%;对于综合飞行换算率,改进算法的综合飞行换算率平均值比确定性方法的结果小1%;且在改进算法下单次飞行换算率和综合飞行换算率服从正态分布.     

多轴随机载荷下的疲劳寿命估算方法

提出了一种多轴随机载荷下的疲劳寿命预测方法.通过雨流计数法对各平面上的剪应变进行循环计数,以统计出的剪应变循环作为多轴疲劳损伤的主要控制参数,将各剪应变循环历程内对应的最大正应力和正应变变程作为多轴疲劳损伤的第二控制参数.根据多轴疲劳寿命模型计算出各平面上的损伤,以最大损伤平面作为多轴随机疲劳的临界平面,通过该临界平面上的损伤计算出多轴随机载荷下的疲劳寿命.采用SNCM630钢,304不锈钢和S45C钢3种金属材料的多轴随机疲劳试验数据对提出的寿命预测方法进行评估和验证.结果表明:疲劳寿命预测结果大都分布在试验结果的2倍分散带之内.     

多种失效模式相关的机构运动可靠度计算方法

机构运动中必然存在多种相关失效模式,多为影响机构运动的各类随机变量函数.为了在机构运动可靠性分析中有效考虑多种相关失效模式的影响,建立了考虑多种失效模式相关条件下的机构运动可靠度计算模型,并实现了对多种失效模式相关条件下的机构运动可靠度计算模型的求解,为考虑多种相关失效模式下的机构运动可靠性分析提供了一种有效途径.以6408滚动轴承为例,进行100 000抽样计算,考虑失效模式相关条件下运动可靠度为95.998 9%.该方法精度较高,具有一定的理论意义和应用价值.