超磁致伸缩执行器热损耗模型与实验

针对高频大电流驱动下超磁致伸缩执行器发热严重影响其有效位移输出精度的问题,采用管式冷却结构措施以抑制执行器温升.根据欧姆定律建立交流(DC)与直流(AC)电同时作用下执行器电阻损耗理论模型,基于麦克斯韦方程推导出磁致伸缩棒内部磁场方程及涡流损耗模型,从复数磁导率虚部出发得出磁致伸缩棒磁滞损耗模型.求解上述模型可知:当驱动频率达到50Hz时,磁致伸缩棒损耗占执行器总损耗5%.通过搭建执行器热特性测试实验台,实验测得执行器损耗与理论计算结果吻合良好;管式冷却具有较好的冷却效果,可将磁致伸缩棒温度控制在50℃以内,其实验结果与有限元仿真结果最大误差为3℃以内,进一步验证热损耗计算公式有效性并为精密超磁致伸缩执行器的设计和应用提供了理论支持.      

巨磁电阻材料（La1-xGdx）2/3Ca1/3MnO3的制备工艺及其结构研究

采用固相反应法制备巨磁电阻材料(La1-xGdx)2/3Ca1/3MnO3和La1-xZnxMnO3.La2/3Ca1/3MnO3样品在1200～1400 ℃等五个不同温度下烧结12h;(La1-xGdx)2/3Ca1/3MnO3(x=0.2,0.4,0.6,0.8,1.0)样品系列在1350℃下分别烧结12h和24h,另外样品La1-xZnxMnO3(x=0.1,0.5,0.9)系列在1350℃下烧结24h.利用X射线衍射(XRD)和扫描电镜(SEM)对各样品晶体结构和表面微观结构进行了研究.X射线衍射结果表明,所有样品晶体结构基本不变,保持钙钛矿结构(空间群为Pnma),但随着掺杂量的增加,样品(La1-xGdx)2/3Ca1/3MnO3和La1-xZnxMnO3系列的晶格常数和晶胞体积发生了变化,并且产生了杂质相,导致对结构很敏感的这些材料的磁电性能发生变化.扫描电镜结果表明,样品La2/3Ca1/3MnO3在1400℃时烧结效果最好.     

超磁致伸缩执行器驱动的射流伺服阀参数优化

为提高射流伺服阀的性能,提出了一种超磁致伸缩执行器驱动的直动式射流伺服阀.采用磁场有限元分析的方法,建立了超磁致伸缩执行器输出电流与输出位移的关系,分析了线圈结构对其输出位移的影响,并给出了所设计执行器的实验曲线.结合所设计的射流伺服阀的特点,以能量传递效率最大为优化目标,建立了射流结构与射流效率的关系方程,求出了所设...     

巨磁致伸缩材料作动器及其谐振频率研究

 快速倾斜镜（FSM）是自适应光学系统中提高系统传输精度的关键器件。针对快速倾斜镜的应用背景,采用巨磁致伸缩材料作为驱动组元,研制适用于新型快速倾斜镜的巨磁致伸缩材料作动器,并对作动器的输出位移、输出力及振动模态进行了研究。采用超高温度梯度区熔定向凝固法制备了具有〈112〉轴向择优取向的TbDyFe巨磁致伸缩合金,其10MPa预压力时平行于外磁场方向的饱和磁致伸缩性能达到0.175%,线性段磁致伸缩性能超过0.12%。所研制的巨磁致伸缩材料作动器的准静态位移超过±40μm,输出力达到1 000N以上,并且具有良好的动态响应。巨磁致伸缩材料作动器在1kg负载时的一阶共振频率达到97Hz。这为新型快速倾斜镜系统的研制建立了良好的基础。     

基于弹性阻尼基座的超磁致伸缩致动器响应模型

为弥补环境引起的超磁致伸缩材料的不可控变形,将超磁致伸缩致动器置于弹性阻尼基座上,计算此时输出端和底座的稳态响应.将系统简化为两自由度线性系统,建立了系统的振动微分方程,计算其固有角频率,并通过简谐激励输入分析了系统的幅频特性.输入不同幅值和频率的简谐电流,通过实验得到输出端和底座的位移;根据实验结果计算了模型的相对误差,并对比模型和实验的绝对误差.计算结果表明:模型与实验结果的相对误差不超过9%,绝对误差不超过0.01mm,由此验证了模型的准确性.      

基于超磁致伸缩材料新型转换器的仿真研究

超磁致伸缩材料作为一种新型功能材料具有应变大,输出力大,响应速度快,能量转换效率高等特点。利用超磁致伸缩材料研制了一种取代两级传统电液伺服阀力矩马达的新型电-机转换器,并建立了其数学模型及MATLAB仿真模型,通过仿真结果分析表明该转换器较传统力矩马达具有高频响、高响应等显著优点。     

Exoplanetary searches with gravitational microlensing: Polarization issues

There are different methods for finding exoplanets such as radial spectral shifts, astrometrical measurements, transits, timing etc. Gravitational microlensing (including pixel-lensing) is among the most promising techniques with the potentiality of detecting Earth-like planets at distances about a few astronomical units from their host star or near the so-called snow line with a temperature in the range 0–100 ^°C on a solid surface of an exoplanet. We emphasize the importance of polarization measurements which can help to resolve degeneracies in theoretical models. In particular, the polarization angle could give additional information about the relative position of the lens with respect to the source.     

Geology of the Icy Satellites

In the last 25 years, the explorations of the Voyager and Galileo missions have resulted in an entirely new view of the icy worlds orbiting the giant outer planets. These objects show a huge diversity in their characteristics, resulting from their formation histories, internal processes and interactions with their space environments. This paper will review the current state of knowledge about the icy satellites and discuss the exciting prospects for the upcoming Cassini/Huygens mission as it begins a new era of exploration of the Saturn satellite system.     

Neutral Atmospheres of the Giant Planets: An Overview of Composition Measurements

Measurements of the chemical composition of the giant planets provide clues of their formation and evolution processes. According to the currently accepted nucleation model, giant planets formed from the initial accretion of an icy core and the capture of the protosolar gas, mosly composed of hydrogen and helium. In the case of Jupiter and Saturn (the gaseous giants), this gaseous component dominates the composition of the planet, while for Uranus and Neptune (the icy giants) it is only a small fraction of the total mass. The measurement of elemental and isotopic ratios in the giant planets provides key diagnostics of this model, as it implies an enrichment in heavy elements (as well as deuterium) with respect to the cosmic composition. Neutral atmospheric constituents in the giant planets have three possible sources: (1) internal (fromthe bulk composition of the planet), (2) photochemical (fromthe photolysis ofmethane) and(3) external (from meteoritic impacts, of local or interplanetary origin). This paper reviews our present knowledge about the atmospheric composition in the giant planets, and their elemental and istopic composition. Measurements concerning key parameters, like C/H, D/H or rare gases in Jupiter, are analysed in detail. The conclusion addresses open questions and observations to be performed in the future.     

Comparative Study of the Dynamics of the Outer Planets

The two classes of outer planets, Gas Giants and Ice Giants, have distinctly different global circulation patterns and internal structure. Ongoing ground-based observations of the Ice Giants provide clues to better understanding and Galileo and Cassini data will generate constraints for Gas Giant modeling. The composition below the cloud levels, the depths to which the winds penetrate and the processes that sustain the zonal winds and weather systems are not understood. Basic questions concerning the structure, composition and atmospheric dynamics that are sustained on the four giants could be answered by a combination of orbiters and probes. Future missions that could answer these questions are not currently under development.