单体引入方式对聚苯乙烯微球粒径分布的影响

利用分散聚合技术,采用单体滴加法合成了具有优良单分散性的3.8~7.1μm聚苯乙烯微球。研究了不同单体引入方式对所制备微球的形貌、粒径及粒径分布的影响。发现在最佳滴加速率下,单体滴加法所制备微球的分散系数均小于4.8%,单分散性远高于一次引入法所制备的微球。结合聚合反应动力学研究,阐明了单体滴加法的反应机理及滴加速率的影响规律。结果表明单体滴加法是制备高单分散性的3.8~7.1μm聚苯乙烯微球的有效方法。     

大粒径聚苯乙烯微球的悬浮聚合反应历程研究

采用悬浮聚合方法制备了粒径约为100~120μm的聚苯乙烯(PS)微球。通过在聚合过程中逐步取样,并结合扫描电子显微镜(SEM)及光学显微镜(OM)等手段研究了样品在不同聚合时期中的微观形貌、粒径及其分布的情况,讨论了悬浮聚合制备大粒径PS微球的反应历程。结果表明:大粒径PS微球的悬浮聚合过程主要经历3阶段:液—液分散期、粒子增长期和粒子恒定期,在特定的聚合时期,微球的生长方式和微观形貌有显著不同。在不同生长时期内通过对聚合反应条件的选择性调节,可实现对最终PS微球的形貌、粒径及其分布的有效控制。     

胶凝剂对NiFe2O4纳米粉末制备及磁性能的影响

采用溶胶一凝胶法制备NiFe2O4纳米粉末，胶凝剂分剐采用柠檬酸和PEG200，测定了样品的TG-DTA曲线、红外吸收光谱、X射线衍射谱和磁性能。结果表明，采用不同的胶凝剂，NiFe2O4纳米粉末制备过程中出现明显不同的物理和化学变化；200℃以上的热处理促进粉末的长大和晶化过程，随着温度的升高，晶化程度增强，粉末粒径增大；NiFe2O4纳米粉末的磁性能与热处理温度、粉末的粒径大小及磁性测量样品装载条件等密切相关。     

聚苯胺中空微球的改性与电磁特性

 用分散聚合法制备单分散的聚苯乙烯（PS）微球，并用浓硫酸对PS微球进行表面改性。将改性后的PS微球作为制备聚苯胺（PANI）中空微球的模板，在一定浓度HCl掺杂条件下，苯胺单体在PS模板表面聚合，然后将PS模板通过N，N 二甲基甲酰胺(DMF)溶解，得到了粒径在0.8~1.2 μm的PANI中空微球。若在PANI聚合过程中加入适量的Fe₃O₄,可获得由Fe₃O₄与PANI构成的复合中空微球。2~18 GHz的波导法测试结果表明，经HCl和Fe₃O₄掺杂后的复合中空微球与本征态PANI中空微球的电磁参数存在很大变化；吸波性能研究表明，8~12 GHz范围内，PANI中空微球的吸波效果要好于其实心微球的吸波效果。     

Ag包覆弹性体微球的制备及其电性能

采用置换反应法和化学沉积法制备了微米级镀Ag丙烯酸酯橡胶（ACM）微球，研究了镀Ag导电弹性体微球的电性能。结果表明：置换反应法通过对微球基体先化学镀铜再置换镀Ag，能够得到镀层均匀致密、包覆完善的镀Ag弹性体微球；所制备镀Ag微球的体积电阻率随外加压力及温度的升高，均呈现规律性降低，并且不受热循环的影响，表明所制备的镀Ag导电弹性体微球具有一定的弹性、热膨胀性以及良好的热稳定性。     

磁研磨法对钛合金弯管内表面的抛光研究

航空发动机中所使用的钛合金弯管在加工时其内表面会产生微裂纹、褶皱等缺陷,用传统的研磨工艺难以实现对弯管内表面的抛光处理,而磁力研磨加工工艺却可以很好地解决这一难题。利用磁力线可以穿透钛合金弯管的特性,磁性磨料可以在外加磁场的作用下压附在弯管内表面,并随磁场高速旋转与弯管内表面产生相对运动,从而达到研磨钛合金弯管内表面的目的。本文对磁研磨法加工钛合金弯管内表面的研磨原理及磁性研磨颗粒的受力情况进行了的分析,并通过详细的试验研究得出:钛合金弯管内表面经过研磨后,原有的微裂纹、褶皱等缺陷得到明显改善,表面粗糙度值由R_a0.35μm降低到R_a0.12μm,验证了磁研磨法对钛合金弯管内表面的研磨抛光起到的良好效果。     

PS/CeO_2核壳型复合磨粒的微晶玻璃抛光试验研究

为获得同时具有低表面粗糙度和高面形精度的微晶玻璃基片,利用PS(聚苯乙烯)微球和CeO2磨粒制备出核壳型复合磨粒,替代了单一CeO2磨粒进行抛光试验。通过全因子试验研究PS微球粒径和质量浓度对微晶玻璃基片的材料去除率(MRR)、表面粗糙度和面形精度的影响。试验表明:MRR随着PS微球质量浓度的增大而减小,随着PS微球粒径的增大而增大;PS微球粒径为20μm时,工件塌边显著减小;表面粗糙度随着PS微球浓度的增大而增大。     

交联淀粉微球的反相悬浮合成及成粒机理

以可溶性淀粉为原料,Span60和Tween60为分散剂,N和N-亚甲基双丙烯酰胺(MBAA)为交联剂,利用反相悬浮聚合法合成淀粉微球,分析反应时间、反应温度、引发剂用量、交联剂用量对淀粉微球溶胀度和平均粒径的影响规律,并探讨CSMs的成粒机理。     

钴的晶体结构对镀钴空心玻璃微球电磁性能的影响

采用化学镀方法在空心玻璃微球表面复合磁性金属钴,制备了镀钴空心玻璃微球,并对其进行了真空退火热处理。经过化学镀的空心玻璃微球表面包覆了一层均匀、致密的金属镀层;镀钴空心玻璃微球(2.5g/cm3)镀层晶体结构对其电磁性能产生影响。当镀层Co含量为95%时,介电常数实部在11GHz处达到35,虚部在13GHz处达到22;在经过热处理后,镀层发生晶相转变,介电常数实部和虚部均得到提高。另外,热处理能降低钴镀层的矫顽力,改善其软磁性能。     

基于MATLAB下的磁性测量新方法

在简单介绍磁性测量冲击法基本原理的基础上,提出了一种将多元回归分析应用于磁性测量中的新方法。着重讲述了如何实现基于多元回归分析法下的磁性测量新方法,借助于MATLAB语言编辑可实现多元回归算法及磁测新方法的多个可嵌套调用的GUI界面。实践证明,使用MATLAB可实现磁性测量新方法,该方法大大缩短了测量周期,所编辑的GUI界面充分利用了MATLAB函数库,可快速精确的处理磁测数据,建立回归模型,保存并显示计算结果,且操作方便。     

聚合物/纳米复合材料的制备、性能及其应用展望

介绍了纳米粒子的表面效应、小尺寸效应、量子尺寸效应等特性，聚合物/纳米复合材料的概念和结构性能；综述了聚合物/纳米复合材料的几种常用制备方法；总结了由于纳米粒子的存在聚合物/纳米复合材料在力学、光、电、磁等方面呈现出常规材料不具备的特性，并结合其特性展望了聚合物/纳米复合材料的应用前景。     

实用化光力加速度计中单微球重复起支技术

针对光力加速度计的小型化应用,设计并制作了一种基于V型槽的片上光纤光阱,并采用机械振动方法实现了单微球重复起支。理论研究了利用机械振动方法实现微球起支、捕获的动力学过程。结果表明,只有当微球脱离捕获室底面的初始速度满足一定范围时才能稳定捕获,该初始速度范围与捕获室的几何参数有关。提出了利用两光纤中相向传播光的耦合功率监测微球捕获状态的方法,并通过实验完成了微球起支过程的自动控制,实现了单微球的重复起支与捕获。该片上光纤光阱制备方法和单微球重复起支技术可推动光力加速度计的实用化进程。     

先进树脂基复合材料的发展

先进树脂基复合材料在过去三十年中已得到了飞速的发展.本文主要介绍了它们的发展现状及在航空工业的应用,讨论了先进树脂基复合材料的未来研究和发展方向以及应注意的几个问题.     

实用化光力加速度计中单微球重复起支技术

针对光力加速度计的小型化应用，设计并制作了一种基于V型槽的片上光纤光阱，并采用机械振动方法实现了单微球重复起支。理论研究了利用机械振动方法实现微球起支、捕获的动力学过程。结果表明，只有当微球脱离捕获室底面的初始速度满足一定范围时才能稳定捕获，该初始速度范围与捕获室的几何参数有关。提出了利用两光纤中相向传播光的耦合功率监测微球捕获状态的方法，并通过实验完成了微球起支过程的自动控制，实现了单微球的重复起支与捕获。该片上光纤光阱制备方法和单微球重复起支技术可推动光力加速度计的实用化进程。     

Small-scale solar magnetic fields: An overview

An overview is given of the observational and the theoretical methods used to investigate solar magnetic fields. It includes an introduction to the Stokes parameters, their radiative transfer in the presence of a magnetic field, and empirical techniques used to measure various properties of solar magnetic features, such as the strength and direction of the magnetic field, magnetic flux, temperature, velocity, size and lifetime. The MHD equations are introduced and some of the most common simplifications used to describe solar magnetic features are outlined.The application of these techniques to small-scale magnetic features is surveyed. The results of empirical and theoretical investigations of small-scale solar magnetic features are reviewed. Current views on their magnetic structure, thermal stratification, velocity field, size, distribution and evolution are presented. Finally, some open questions concerning small-scale solar magnetic fields are listed.     

Electromagnetic Induction Effects and Dynamo Action in the Hermean System

Embedded in a large mass density and strong interplanetary magnetic field solar wind environment and equipped with a magnetic field of minor strength, planet Mercury exhibits a small magnetosphere vulnerable to severe solar wind buffeting. This causes large variations in the size of the magnetosphere and its associated currents. External fields are of far more importance than in the terrestrial case and of a size comparable to any internal, dynamo-generated field. Induction effects in the planetary interior, dominated by its huge core, are thought to play a much more prominent role in the Hermean magnetosphere compared to any of its companions. Furthermore, the external fields may cause planetary dynamo amplification much as discussed for the Galilean moons Io and Ganymede, but with the ambient field generated by the dynamo and its magnetic field-solar wind interaction.     

The Feasibility of Packaging High-Frequency Microcircuits Inside the Magnetic Core

A design goal for miniaturization has long been the elimination of the magnetic circuit. In practice, the size/weight penalties are decreased by operation at higher frequency where core size can be effectively reduced. When microcircuitry is considered, the magnetic circuit is designed out. Either RC or active networks replace inductance, or it is externally added to the microcircuit. This paper will demonstrate that the microcircuit elements can be readily interconnected inside of ferrite pot cores. Linear circuits using the magnetic circuit to advantage can be packaged in the same volume as the transformer, inductance, or filter alone. The natural RFI and radiation shielding, as well as heat transfer capabilities, are inherent with this form of packaging. For illustration, a 2-kV, 20-?A power supply featuring a 60-kHz, class C oscillator; a 10-volt, 100-mA converter featuring a 300-kHz square-wave oscillator; and a 9.5-volt, 100-mA switching regulator are packaged inside ferrite pot cores. With this technique only functional input-output connections are necessary, since the microcircuitry interconnections are inside the pot core.     

磁流体密封结构参数对密封能力的影响

在采用磁场分析法, 并利用不等间距网格的有限差分数值方法对磁流体密封装置中稳态磁场进行分析 [3] 的基础上, 研究了矩形齿磁流体密封装置结构参数对密封能力的影响, 并根据磁路分析方法定性解释了参数对密封能力的影响规律 (参数包括密封间隙、极齿结构参数、永磁体结构参数以及极齿齿数)。根据分析计算的结果, 对磁流体密封进行了优化设计和实验验证, 优化设计出的装置体积和重量降低了50%以上。      

航空铁磁材料磁记忆检测新方法

 为提高现有磁记忆检测方法的可靠性,充分考虑各向磁记忆信号分量特征,提出法向和切向相结合的磁记忆检测新方法,对航空铁磁材料18CrNi4A试件在不同拉伸载荷下同时采集法向和切向两个方向上的磁记忆信号,并对信号进行小波包滤波处理后取李萨如图,用图中封闭区域出现的位置判断应力集中部位,用封闭区域面积的大小判断应力集中程度,研究磁记忆信号法向分量和切向分量联合检测材料的应力状态。结果表明:对该材料试件磁记忆信号法向分量和切向分量进行小波包降噪方法切实可行,处于应力集中试件的磁记忆信号反映在李萨如图上会出现封闭区域,并且随着应力集中程度的增大,李萨如图上封闭区域的面积有增大趋势,材料出现明显屈服后,面积增大得更加明显。该方法具有一定的工程实际应用价值。     

The IMF pile-up regions near the Earth and Venus: lessons for the solar wind - Mars interaction

The Mars Global Surveyor mission has revealed that localized crustal paleomagnetic anomalies are a common feature of the Southern Hemisphere of Mars. The magnetometer measured small-scale magnetic fields associated with many individual magnetic anomalies have magnitudes ranging from hundreds to thousands nT at altitude above 120 km. That makes Mars globally different from both Venus and Earth. The data collected by Lunar Prospector near the Moon were interpreted as evidence that above regions of inferred strong surface magnetic fields on the Moon the SW flow is deflected, and a small-scale mini-magnetosphere exists under some circumstances. With a factor of 100 stronger magnetic fields at Mars and a lower SW dynamic pressure, those conditions offer the opportunity for a larger size of small `magnetospheres' which can be formed by the crustal magnetic fields. Outside the regions of the magnetic anomalies, the SW/Mars interaction is Venus-like. Thus, at Mars the distinguishing feature of the magnetic field pile-up boundary most likely varies from Venus-like to Earth-like above the crustal magnetic field regions. The observational data regarding the IMF pile-up regions near Venus and the Earth are initially reviewed. As long as the SW/Mars interaction remains like that at Venus, the IMF penetrates deep into the Martian ionosphere under the `overpressure' conditions. Results of numerical simulations and theoretical expectations regarding the temporal evolution of the IMF inside the Venus ionosphere and appearance of superthermal electrons are also reviewed and assessed.