氧化铝基吸波材料研究进展

雷达波吸收材料在国防领域发挥着重要的作用。厚度薄、密度低、吸收频带宽、吸收强是当前吸波材料的研究重点。高马赫飞行的武器装备会因空气阻力而使机体局部温度很高,常温吸波材料不适用,亟待研究耐高温并高效吸收电磁波的吸波材料。以氧化铝为基体,复合不同类型吸收剂制备的高温吸波材料已被广泛关注与研究。本文系统总结近年来金属(合金)/氧化铝复合吸波材料、非金属/氧化铝复合吸波材料、其他含氧化铝复合吸波材料的研究现状,对不同结构(纳米线、微球及纳米颗粒等)吸收剂与多种形态(多孔膜、纤维或纳米颗粒)氧化铝基体制备的复合吸波材料的结构、性能和吸波机理进行了分析,并对金属(合金)/氧化铝复合吸波材料及非金属/氧化铝复合吸波材料的发展方向做出展望。在金属(合金)/氧化铝复合吸波材料方面应加强:(1)开发纳米级的球形超细金属吸收剂,利用纳米粒子的特殊效应来提高吸波性能;(2)进一步探索合理的制备工艺,达到吸收剂与基体良好匹配。在非金属/氧化铝复合吸波材料方面:(1)进一步加强氧化铝纤维布和氧化铝网状基体与纳米吸波剂复合的研究;(2)加强高分子特殊核壳结构、阻抗匹配层等方面的研究;(3)加强宽频吸波材料及吸波剂改性增强吸波材料的研究;(4)开展金属氧化物粉体与无机黏结剂组成的无机基体方面研究。     

碳团簇复合吸波材料的结构设计与性能

通过物理和化学方法制得聚丙烯腈(PAN)基碳团簇复合吸波材料,利用SEM和XRD对其结构及形貌进行了表征,并以碳团簇复合吸波材料和碳团簇材料分别为吸收剂制备的吸波涂层进行了吸波性能测试。结果表明:以碳团簇复合吸波材料为吸收剂制备的吸波涂层带宽要优于以碳团簇材料为吸收剂制备的吸波涂层,该碳团簇复合吸波材料兼具电和磁损耗的能力。     

吸波型SiC陶瓷材料的研究进展

随着电子产品的广泛应用,电磁波泄露和干扰成为普遍问题,迫切需要发展新一代高性能吸波材料。SiC陶瓷及陶瓷基复合材料具有耐高温、耐腐蚀、抗氧化、高强度、低密度、介电性能可设计等优异特性,是极具潜力的吸波型热结构材料。化学气相渗透和先驱体转化陶瓷法可实现陶瓷材料的微结构设计,是制备高性能吸波型热结构陶瓷的主要方法,日益受到关注。本文综述了吸波型热结构陶瓷的设计与制备方法及其吸波机理。     

高温雷达吸波涂层研究进展

在现代信息化战争中,探测和制导技术迅猛发展。在众多探测信号中,雷达探测占比高达60%,因此武器装备雷达隐身 能力尤其重要。随着新一代装备性能的提升,热端部件的服役温度不断升高,对高温雷达吸波涂层提出了更加严苛的要求。在高 温服役环境下,部分雷达吸波材料存在氧化、居里温度低而失去吸波性能的问题。高温雷达吸波材料主要依靠介电损耗和电导损 耗机制实现对电磁波的损耗吸收。基于此,综述了以碳化物、硼化物、氧化物、金属材料、MAX相材料为吸波剂的高温雷达吸波涂 层研究情况,分析了各材料的优势及存在的问题,其中氧化物吸波剂高温稳定性好,易于制备,成本低,其吸波性能可通过掺杂改 性调控,是面向未来更加严苛服役环境下更具应用潜力的吸波材料。此外,还从梯度结构和超材料设计2个角度分析了涂层结构 设计在拓宽涂层吸波频带,降低涂层厚度方面的作用。结合当前研究进展提出了新材料研发、新结构设计和与材料结构相适应的 制备工艺研究是未来高温雷达吸波涂层的发展方向。     

耐高温陶瓷基结构吸波复合材料研究进展

陶瓷基结构吸波复合材料具有耐高温、耐腐蚀、抗氧化等诸多优点,是解决武器装备热端隐身问题的关键材料,具有重要应用前景和战略意义。本文介绍了陶瓷吸波材料的微观-宏观多级设计方法,综述了掺杂改性碳化硅陶瓷、钡铁氧体陶瓷、聚合物转化陶瓷(PDCs)、3D打印多孔陶瓷及陶瓷蜂窝、连续纤维增强陶瓷基复合材料(CFCMC)等新型陶瓷基复合材料的最新研究进展,展望了结构吸波一体化的陶瓷基复合材料的发展趋势,提出微观-宏观多级结构设计的纤维增强陶瓷基复合材料将是未来高温隐身材料领域的重要发展方向。     

雷达吸波材料和吸波结构与飞机隐身技术

雷达吸波材料和吸波结构的使用是飞机隐身的一个重要措施。本文介绍了雷达吸波材料(RAM)和吸波结构(RAS)及其在飞机隐身技术中的作用。     

高熵陶瓷:吸波材料设计新策略北大核心CSCD

微波技术的进步促进了电磁防护技术的发展。吸波材料可以将过剩的电磁辐射以热量形式耗散,因此受到了广泛关注。面对复杂的电磁环境,寻找在1~18 GHz频段内兼具强吸收和宽频吸收性能的吸波材料具有重要意义。目前,吸波材料的设计方法主要包括制备纳米复相材料和掺杂改性。通过将介电损耗型和磁损耗型的材料在纳米尺度复合可以实现两种损耗机制的耦合,但制备工艺复杂、纳米填料分散性难以精确控制、高温热稳定性及抗氧化性差等问题是制约纳米复相材料应用的主要因素。超高温陶瓷具有高温热稳定性及抗氧化性好等优点,但阻抗匹配差使其难以作为吸波材料应用。通过设计和制备含有磁性组元的高熵陶瓷可以使超高温陶瓷材料兼具宽频吸收和强吸收的高效吸波性能。采用高熵设计方法可以同时调节导电性和增强磁损耗能力,为导电性良好的介电型吸波材料提供了调控阻抗匹配的新思路。     

CNTs泡沫相变复合材料:纳米孔隙的构筑与相变材料的包裹

热能是一种广泛存在并极具应用前景的能源,但目前储热材料的能量转换时间较长,储热效率较低,亟需一种高性能的新型储热材料。本工作通过化学气相沉积(chemical vapor deposition,CVD)方法利用碳纳米管(carbonnanotubes,CNTs)构筑宏观体材料,在微纳尺度下对复合材料结构进行优化,合成孔隙结构可控的 CNTs泡沫,利用毛细管作用力将熔融相变材料硬脂酸和石蜡填充到 CNTs 泡沫中,形成分散均匀的 CNTs相变复合材料。用聚焦离子/电子双束显微电镜(FIB/SEM)观察样品形貌,用差式扫描量热计(DSC)分析样品潜热,用 X 射线衍射仪(XRD)分析样品晶体结构,用拉伸试验机测试样品强度。结果表明:CNTs泡沫对相变材料具有优异的包裹性,减少了在相变循环中相变材料的流失;复合相变材料具有较高的潜热。     

雷达吸波材料设计理论与方法研究进展

综述了近10年来雷达吸波材料(RAM)计算设计理论、方法及优化技术的发展,并简要评价了现有的设计技术。此外,提出了雷达吸波材料设计存在的技术问题,并预测了吸波材料设计的发展方向。     

化学气相渗透制备SiCp/SiC复合材料

在颗粒陶瓷基复合材料中引入一种颗粒团结构,探索了此结构的跨尺度、非均匀复合效应对颗粒陶瓷基复合材料的力学性能影响.采用造粒的方法制备了SiC颗粒团聚体,并利用此颗粒团聚体压制成疏松预制体;采用化学气相渗透(chemical vapor infiltration,CVI)制备SiC基体,并研究了这种复合材料的微结构与力学性能的关系.     

捷变频磁控管用高频直线振荡电机设计

捷变频磁控管的快速捷变特性取决于驱动电机的性能,要求电机功耗小、体积小、效率高,能实现高频稳幅直线振动.文章介绍了音圈直线电机、电磁开关式直线电机和电磁混合式直线电机等三种方案,通过对其工作原理和性能特点分析,确定了音圈直线电机驱动方案,进行了电磁场仿真分析和电磁参数设计,进行了样机试验测试.结果表明,设计的音圈直线电...     

桨叶实度及轴间距对摆线桨气动特性影响研究

悬停状态下,设计参数和摆线桨间距离对摆线桨的气动特性有较大影响。首先通过算例验证滑移网格计算方法应用于摆线桨悬停状态下气动力计算的准确性,然后研究摆线桨在不同半径、弦长和桨叶数时的气动参数特性,最后计算分析不同距离时,摆线桨间的气动干扰特性。结果表明:随着半径增大,桨叶气动力和单位面积上载荷均增大;弦长越大,气动力越大,桨叶单位面积上载荷反而越小;4叶片摆线桨产生的气动力比3叶片和6叶片大,而3叶片的桨叶载荷最大;合力偏转角分别随转速和实度的增大而减小;随着摆线桨间距离的增加,气动力损失系数和合力偏转角均减小。     

A new target tracking filter based on deep learning

At present, current filters can basically solve the filtering problem in target tracking, but there are still many problems such as too many filtering variants, too many filtering forms, loosely coupled with the target motion model, and so on. To solve the above problems, we carry out crossapplication research of artificial intelligence theory and methods in the field of tracking filters. We firstly analyze the computation graphs of typical a-β and Kalman. Through analysis, it is concluded that ...     

Investigations of entrainment characteristics and shear-layer vortices evolution in an axisymmetric rear variable area bypass injector

In this study,firstly,for the axisymmetric RVABI,the change-rule of adverse pressure gradient caused by radial velocity during the transition of internal flow mode in variable geometry is summarized,and a Bypass Ratio(BR) iterative algorithm based on the empirical correlation of non-equilibrium pressure is proposed.The algorithm can estimate the nonlinear relationship between area ratio and BR,with an error range falling below 6.5%.Then,we discuss the favorable effect of uniform mixing on the th...     

PVC糊树脂对交联PVC泡沫塑料的影响

通过水煮发泡制备交联聚氯乙烯泡沫塑料,讨论了聚氯乙烯(PVC)糊树脂对泡沫制备过程中经制糊、模压和发泡工艺得到的产物的影响,研究了PVC糊树脂对制备的交联PVC泡沫压缩性能的影响.结果表明:制备交联聚氯乙烯泡沫塑料适宜的糊黏度是4～9 Pa·s;PVC糊树脂的K值较大或水萃取液pH值呈碱性可有效防止模压过程中PVC的降解;PVC糊树脂的水萃取液pH值呈碱性可催化发泡反应,有利于得到低密度泡沫且缩短发泡时间;随着其K值增加,制备的泡沫压缩强度增大,但是K值过大时,制备的泡沫泡孔较大,压缩强度反而降低,适宜的K值为70～80.     

Alfvénic Electron Acceleration in Aurora Occurs in Global Alfvén Resonosphere Region

Auroral emission caused by electron precipitation (Hardy et al., 1987, J. Geophys. Res. 92, 12275–12294) is powered by magnetospheric driving processes. It is not yet fully understood how the energy transfer mechanisms are responsible for the electron precipitation. It has been proposed (Hasegawa, 1976, J. Geophys. Res. 81, 5083–5090) that Alfvén waves coming from the magnetosphere play some role in powering the aurora (Wygant et al., 2000, J. Geophys. Res. 105, 18675–18692, Keiling et al., 2003, Science 299, 383–386). Alfvén-wave-induced electron acceleration is shown to be confined in a rather narrow radial distance range of 4–5 R _E (Earth radii) and its importance, relative to other electron acceleration mechanisms, depends strongly on the magnetic disturbance level so that it represents 10% of all electron precipitation power during quiet conditions and increased to 40% during disturbed conditions. Our observations suggest that an electron Landau resonance mechanism operating in the “Alfvén resonosphere” is responsible for the energy transfer.     

Multiframe weak target track-before-detect based on pseudo-spectrum in mixed coordinates

Traditional multiframe Track-Before-Detect(TBD) may incur adverse integration loss resulting from model mismatch in sensor coordinates. Its suboptimal integration strategy may cause target envelope degradation. To address these issues, a pseudo-spectrum-based multiframe TBD in mixed coordinates is proposed firstly. The data search for energy integration is conducted based on an accurate model in the x-y plane while target energy is integrated based on pseudo-spectrum in sensor coordinates. The a...     

Deep Impact: Working Properties for the Target Nucleus – Comet 9P/Tempel 1

In 1998, Comet 9P/Tempel 1 was chosen as the target of the Deep Impact mission (A’Hearn, M. F., Belton, M. J. S., and Delamere, A., Space Sci. Rev., 2005) even though very little was known about its physical properties. Efforts were immediately begun to improve this situation by the Deep Impact Science Team leading to the founding of a worldwide observing campaign (Meech et al., Space Sci. Rev., 2005a). This campaign has already produced a great deal of information on the global properties of the comet’s nucleus (summarized in Table I) that is vital to the planning and the assessment of the chances of success at the impact and encounter. Since the mission was begun the successful encounters of the Deep Space 1 spacecraft at Comet 19P/Borrelly and the Stardust spacecraft at Comet 81P/Wild 2 have occurred yielding new information on the state of the nuclei of these two comets. This information, together with earlier results on the nucleus of comet 1P/Halley from the European Space Agency’s Giotto, the Soviet Vega mission, and various ground-based observational and theoretical studies, is used as a basis for conjectures on the morphological, geological, mechanical, and compositional properties of the surface and subsurface that Deep Impact may find at 9P/Tempel 1. We adopt the following working values (circa December 2004) for the nucleus parameters of prime importance to Deep Impact as follows: mean effective radius = 3.25± 0.2 km, shape – irregular triaxial ellipsoid with a/b = 3.2± 0.4 and overall dimensions of ∼14.4 × 4.4 × 4.4 km, principal axis rotation with period = 41.85± 0.1 hr, pole directions (RA, Dec, J2000) = 46± 10, 73± 10 deg (Pole 1) or 287± 14, 16.5± 10 deg (Pole 2) (the two poles are photometrically, but not geometrically, equivalent), Kron-Cousins (V-R) color = 0.56± 0.02, V-band geometric albedo = 0.04± 0.01, R-band geometric albedo = 0.05± 0.01, R-band H(1,1,0) = 14.441± 0.067, and mass ∼7×10¹³ kg assuming a bulk density of 500 kg m⁻³. As these are working values, {i.e.}, based on preliminary analyses, it is expected that adjustments to their values may be made before encounter as improved estimates become available through further analysis of the large database being made available by the Deep Impact observing campaign. Given the parameters listed above the impact will occur in an environment where the local gravity is estimated at 0.027–0.04 cm s⁻² and the escape velocity between 1.4 and 2 m s⁻¹. For both of the rotation poles found here, the Deep Impact spacecraft on approach to encounter will find the rotation axis close to the plane of the sky (aspect angles 82.2 and 69.7 deg. for pole 1 and 2, respectively). However, until the rotation period estimate is substantially improved, it will remain uncertain whether the impactor will collide with the broadside or the ends of the nucleus.     

Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R _S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm² sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5^∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm² sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm² sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm² sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R _S every 2–3 h (every ∼10 min from ∼20 R _S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date.