共查询到19条相似文献,搜索用时 140 毫秒
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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。 相似文献
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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。 相似文献
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王旭东%何世禹%杨德庄%魏鹏飞 《宇航材料工艺》2002,32(1):12-18
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。 相似文献
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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. 相似文献
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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。 相似文献
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Bela G. Fejer 《Space Science Reviews》2011,158(1):145-166
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. 相似文献
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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. 相似文献
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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。 相似文献
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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. 相似文献
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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. 相似文献
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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. 相似文献
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动量轮在轨状态可靠性贝叶斯网络建模与评估 总被引:4,自引:1,他引:3
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。 相似文献