电磁式头盔瞄准具指向解算的一种新方法

 <正> 1.引言 电磁感应式头盔瞄准具是近年来发展起来的既适用于飞机又适用于地面火控瞄准的一种新型瞄准装置,其关键部分为电磁敏感系统,主要依靠两个三轴天线的空间场量与空间位置关系来获得瞄准方向。两个三轴天线均由3个相互正交的环天线组成,一个称为辐射器,一个称为敏感器,以辐射器的三轴为基准(固定于飞机),以敏感器的一轴为瞄准方向(装于头盔),两者的空间位置变化关系可由图1中两坐标系来表示,并与辐射器发射量和敏感器接收量有以下关系式     

德研制可探测宇宙射线小型设备

2010年5月28日，德国两家科研机构报告说，它们合作开发出一种可探测宇宙射线的小型太赫兹激光仪，由于重量轻，该设备可以在科研用飞机上使用，从而方便科学家研究宇宙奥秘。     

三层媒质中电偶极子的仿真

偶极子模型是进行水下电磁场建模的主要手段,研究其在海水中产生的场具有重要的实际意义。针对这个问题,利用镜像法,在空气 -海水 -海底三层模型下,在电磁场唯一性原理的基础上,通过矢量磁位方法分别推导了垂直和水平电偶极子在海水中产生的极低频电磁波的解析表达式。通过该方法推导电磁波表达式的过程更加简单,且各个分量有明确的物理意义。仿真结果表明:水平电偶极子的电场和磁场的所有分量场强均大于垂直电偶极子的分量;水平电偶极子在海深方向具有方向性,而垂直电偶极子没有方向性。这些有益的结论为进一步利用垂直/水平电偶极子进行极低频电磁波研究提供参考。     

电子束焊机电磁聚焦控制系统的优化设计

聚焦电流是电子束焊接过程中一个非常重要的参数,调节聚焦电流可以控制电子束焦点相对于工件的位置,从而获得较好的焊缝截面形貌.研究了一种应用混合集成电路技术实现的恒流源,以适应聚焦系统对恒流源高精度、高温度稳定性和较大电流的需求,满足焊接工件在不同的工作距离下都可获得品质较好的电子束束斑.     

基于ANSYS双向超越离合器的接触强度分析

详细介绍了运用ANSYS软件对双向超越离合器的接触强度分析的各个步骤,并把有限元计算结果与传统的赫兹理论计算结果进行比较,证明了此种分析方法的准确性、可靠性,从而为分析双向超越离合器的接触强度提供了一种实用方法。     

曲面蜂窝板预埋管路辐射器热性能试验研究

针对未来航天器拓展曲面散热面的需要,在国内首次设计并制作了一种将热总线翅片管路预埋在曲面蜂窝板内的可展开辐射器;搭建了常温常压试验台,通过试验过程热像图验证了预埋管路与面板之间的热耦合效果;通过不同散热功率、不同外部散热环境的工况测试,测得预埋管路内工质至辐射器面板的平均传热热阻为0.035 W/℃,结果表明:曲面蜂窝板预埋管路辐射器在工艺方面和换热性能方面都可满足航天器工程应用需求,对飞行器整器热设计具有参考意义。     

载人航天器主动热控系统流体回路的轻量化设计

建立载人航天器热控系统内各组成部分传热和质量的数学物理模型,对热控流体回路进行轻量化设计,并讨论相关参数对优化结果的影响。研究发现,在回路散热任务给定时,回路各组成部分的结构参数和辐射器内的散热管道数都存在最佳值,在该值下回路系统质量达到最轻。随着辐射器散热面积的增加,最优的辐射器内散热管道数减少;在给定辐射器散热面积时,当回路散热任务增加时,回路最优设计质量和辐射器内的最优管道数均增加。     

美国用于空间站辐射器中的热控涂层

综述了六种美国可用于空间站辐射器中的热控涂层。从涂层的性能、价格、质量以及成熟性研究，对这六种热控涂层进行了评价。结果表明，Z－93型热控涂层最适合用于空间站的辐射器中，镀银F－46薄膜型热控涂层次之。     

空间辐射器热分析

在航天飞机温控系统中,空间辐射器是最主要部件。对以航天飞机蒙皮为辐射表面的,单面翼—管式空间辐射器进行了详细的热分析,把平均翼效率代替局部翼效率,利用有限差分的方法对单面翼—管式辐射器进行了性能计算。     

一种脉宽数字快速电磁阀驱动电路的设计

采用强激颤振电流、维持颤振电流及占空比的控制方法,设计了一种驱动电路,使电磁阀在开占空比时强激吸合后迅速降低驱动电流,降低了电磁阀的发热量,提高了电磁阀的响应速度,从而达到电磁阀对燃油流量的精确控制.在脉宽数字快速电磁阀电路设计中使用了为数不多的贴片元器件,实现了电磁阀小型化和高可靠性驱动的控制.     

航空电气电弧、短路危害及保护研究

航空电气电弧、短路可能会导致难以挽回的损失,研究航空电气电弧、短路的危害及其保护措施具有 重要意义。通过试验室搭建民用飞机典型的115V/400Hz三相交流电气线路,选取金属导体作为多余物,采 用试验法对飞机电气电弧、短路故障现象进行研究,验证和分析传统热断路器的工作特性,确认电气电弧、短路 故障对电气线路和设备产生的危害程度;同时,分析三种更好的电气电弧、短路保护方法。结果表明:传统热断 路器仅对短路故障具有保护作用,对电气电弧不能产生保护作用;三种新的保护方法电弧检测和保护时间过 长,电弧已对导线和设备产品造成不可恢复的损坏。     

Low Latitude Ionospheric Electrodynamics

The low latitude ionosphere is strongly affected by several highly variable electrodynamic processes. Over the last two decades ground-based and satellite measurements and global numerical models have been extensively used to study the longitude-dependent climatology of low latitude electric fields and currents. These electrodynamic processes and their ionospheric effects exhibit large ranges of temporal and spatial variations during both geomagnetic quiet and disturbed conditions. Numerous recent studies have investigated the short term response of equatorial electric fields and currents to lower atmospheric transport processes and solar wind-magnetosphere driving mechanisms. This includes the large electric field and current perturbations associated with arctic sudden stratospheric warming events during geomagnetic quiet times and highly variable storm time prompt penetration and ionospheric disturbance dynamo effects. In this review, we initially describe recent experimental and numerical modeling results of the global climatology and short term variability of quiet time low latitude electrodynamic plasma drifts. Then, we examine the present understanding of equatorial electric field and current perturbation fields during periods of enhanced geomagnetic activity.     

紧拉型试样的电位场及其在裂纹扩展试验中的应用

疲劳裂纹扩展是预测结构疲劳寿命所必需的基本力学性能之一,而要取得有用的裂纹扩展速率数据,必有可靠的裂纹检测分析方法。在常温下,直读、柔度、涡流、超声、电阻及电位等方法均可应用,但在航空及其他动力装置用高温材料的试验研究中,则几乎只有紧拉（CT）试样的电位法可供使用。因此,较全面地分析CT型试样的电位分布,探讨优先的试验方案和给出相应的裂纹电位标定函数是非常必要的。     

Physics of Electric Discharges in Atmospheric Gases: An Informal Introduction

A short account of the physics of electrical discharges in gases is given from the viewpoint of its historical evolution and application to planetary atmospheres. As such it serves as an introduction to the papers on particular aspects of electric discharges contained in this issue, in particular in the chapters on lightning and the discharges which in the last two decades have been observed to take place in Earth’s upper atmosphere. In addition to briefly reviewing the early history of gas discharge physics we discuss the main parameters affecting atmospheric discharges like collision frequency, mean free path and critical electric field strength. Any discharge current in the atmosphere is clearly carried only by electrons. Above the lower boundary of the mesosphere the electrons must be considered magnetized with the conductivity becoming a tensor. Moreover, the collisional mean free path in the upper atmosphere becomes relatively large which lowers the critical electric field there and more easily enables discharges than at lower altitudes. Finally we briefly mention the importance of such discharges as sources for wave emission.     

信号安全信息光纤局域网的应用研究

电气化机车牵引电流对信号电缆产生谐波干扰,致使用光缆代替电缆,用网络代替单一的传输线路已成为大势所趋。信号安全信息光纤局域网是光通信技术、计算机技术、网络技术在铁路信号领域中的综合应用,其安全性和可靠性是直接关系到能否应用于铁路现场的重要问题,在对这一问题做了较为祥尽探讨的基础上,提出了提高网络安全性的若干措施。     

Numerical Modeling of the Ring Current and Plasmasphere

Over the last 25 years, considerable scientific effort has been expended in the development of quantitative models of the dynamics of Earth's inner magnetosphere, particularly on studies of the injection of the storm-time ring current and of dynamic variations in the shape and size of the plasmasphere. Nearly all modeling studies of ring-current injection agree that time-varying magnetospheric convection can produce approximately the ion fluxes that are observed in the storm-time ring current, but the truth of that assumption has never been demonstrated conclusively. It is not clear that the actual variations of convection electric fields are strong enough to explain the observed flux increases in ~100 keV ions at the peak of the storm-time ring current. Observational comparisons are generally far from tight, primarily due to the paucity of ring-current measurements and to basic limitations of single-point observations. Also, most of the theoretical models combine state-of-the-art treatment of some aspects of the problem with highly simplified treatment of other aspects. Even the most sophisticated treatments of the sub-problems include substantial uncertainties, including the following: (i) There is still considerable theoretical and observational uncertainty about the dynamics of the large-scale electric fields in the inner magnetosphere; (ii) No one has ever calculated a force-balanced, time-dependent magnetic-field model consistent with injection of the storm-time ring current; (iii) The most obvious check on the overall realism of a ring-current injection model would be to compare its predicted Dst index against observations; however, theoretical calculations of that index usually employ the Dessler-Parker-Sckopke relation, which was derived from the assumption of a dipole magnetic field and cannot be applied reliably to conditions where the plasma pressure significantly distorts the field; (iv) Although loss rates by charge exchange and Coulomb scattering can be calculated with reasonable accuracy, it remains unclear whether wave-induced ion precipitation plays an important role in the decay of the ring current. However, considerable progress could be made in the next few years. Spacecraft that can provide images of large regions of the inner magnetosphere should eliminate much of the present ambiguity associated with single-point measurements. On the theoretical side, it will soon be possible to construct models that, for the first time, will solve a complete set of large-scale equations for the entire inner magnetosphere. The biggest uncertainty in the calculation of the size and shape of the plasmasphere lies in the dynamics and structure of the electric field. It is still not clear how important a role interchange instability plays in determining the shape of the plasmapause or in creating density fine structure.     

Magnetic Fields of the Outer Planets

The rapidly rotating giant planets of the outer solar system all possess strong dynamo-driven magnetic fields that carve a large cavity in the flowing magnetized solar wind. Each planet brings a unique facet to the study of planetary magnetism. Jupiter possesses the largest planetary magnetic moment, 1.55×10²⁰ Tm³, 2×10⁴ times larger than the terrestrial magnetic moment whose axis of symmetry is offset about 10° from the rotation axis, a tilt angle very similar to that of the Earth. Saturn has a dipole magnetic moment of 4.6×10¹⁸ Tm³ or 600 times that of the Earth, but unlike the Earth and Jupiter, the tilt of this magnetic moment is less than 1° to the rotation axis. The other two gas giants, Uranus and Neptune, have unusual magnetic fields as well, not only because of their tilts but also because of the harmonic content of their internal fields. Uranus has two anomalous tilts, of its rotation axis and of its dipole axis. Unlike the other planets, the rotation axis of Uranus is tilted 97.5° to the normal to its orbital plane. Its magnetic dipole moment of 3.9×10¹⁷ Tm³ is about 50 times the terrestrial moment with a tilt angle of close to 60° to the rotation axis of the planet. In contrast, Neptune with a more normal obliquity has a magnetic moment of 2.2×10¹⁷ Tm³ or slightly over 25 times the terrestrial moment. The tilt angle of this moment is 47°, smaller than that of Uranus but much larger than those of the Earth, Jupiter and Saturn. These two planets have such high harmonic content in their fields that the single flyby of Voyager was unable to resolve the higher degree coefficients accurately. The four gas giants have no apparent surface features that reflect the motion of the deep interior, so the magnetic field has been used to attempt to provide this information. This approach works very well at Jupiter where there is a significant tilt of the dipole and a long baseline of magnetic field measurements (Pioneer 10 to Galileo). The rotation rate is 870.536° per day corresponding to a (System III) period of 9 h 55 min 26.704 s. At Saturn, it has been much more difficult to determine the equivalent rotation period. The most probable rotation period of the interior is close to 10 h 33 min, but at this writing, the number is still uncertain. For Uranus and Neptune, the magnetic field is better suited for the determination of the planetary rotation period but the baseline is too short. While it is possible that the smaller planetary bodies of the outer solar system, too, have magnetic fields or once had, but the current missions to Vesta, Ceres and Pluto do not include magnetic measurements.     

Electron Acceleration in the Heliosphere

We review the evidence for electron acceleration in the heliosphere putting emphasis on the acceleration processes. There are essentially four classes of such processes: shock acceleration, reconnection, wave particle interaction, and direct acceleration by electric fields. We believe that only shock and electric field acceleration can in principle accelerate electrons to very high energies. The shocks known in the heliosphere are coronal shocks, traveling interplanetary shocks, CME shocks related to solar type II radio bursts, planetary bow shocks, and the termination shock of the heliosphere. Even in shocks the acceleration of electrons requires the action of wave particle resonances of which beam driven whistlers are the most probable. Other mechanisms of acceleration make use of current driven instabilities which lead to electron and ion hole formation. In reconnection acceleration is in the current sheet itself where the particles perform Speiser orbits. Otherwise, acceleration takes place in the slow shocks which are generated in the reconnection process and emanate from the diffusion region in the Petschek reconnection model and its variants. Electric field acceleration is found in the auroral zones of the planetary magnetospheres and may also exist on the sun and other stars including neutron stars. The electric potentials are caused by field aligned currents and are concentrated in narrow double layers which physically are phase space holes in the ion and electron distributions. Many of them add up to a large scale electric field in which the electrons may be impulsively accelerated to high energies and heated to large temperatures.     

动量轮在轨状态可靠性贝叶斯网络建模与评估

卫星动量轮在轨运行环境复杂,并且无失效数据,难以利用传统方法进行可靠性建模与评估。为此,提出一种利用贝叶斯网络融合动量轮各种试验信息及轴温和电流等遥测数据的可靠性建模与评估方法。基于失效分析建立贝叶斯网络拓扑结构,根据试验数据估计网络参数,而后,通过贝叶斯网络的推理得到动量轮可靠度的点估计和区间估计,并利用在轨遥测数据实时评估动量轮可靠性,获得动量轮可靠性变化趋势比较明显的遥测数据取值区间。该方法对动量轮实时状态监控具有一定的理论和实践意义。