NiCo/Cu多层纳米线的制备、表征以及磁化反转机制研究

采用电化学沉积在多孔氧化铝模板中制备了NiCo/Cu多层结构纳米线,并使用扫描电子显微镜(SEM)和透射电子显微镜(TEM)表征了纳米线的形貌和微观结构。透射电子显微镜的结果表明,通过控制阶梯电位时间,制备的铁磁层厚度为100nm,非铁磁层厚度为10nm。结合选区电子衍射技术(SAED)与X射线衍射分析技术(XRD),确定多层纳米线的晶格结构是面心立方(FCC)。在分析多层纳米阵列的微观结构之后,使用振动样品磁强计(VSM)测量磁滞回线。结果表明,随着Co含量的增加,多层纳米线的矫顽力升高。当多层纳米线中Co含量为10%和30%时,易磁化轴垂直于纳米线,当Co含量为70%和90%时,易磁化轴平行于纳米线。最后,对纳米线磁化翻转机制进行微磁学模拟分析得出,当外加磁场垂直于纳米线时,磁化反转机制是形核机制;当外加磁场平行于纳米线时,磁化反转机制是卷曲机制。     

高长径比银纳米线的制备及其透明导电薄膜性能

为改善产品长径比,本文在经典多元醇法的基础上,经过常压滴注路线和密闭溶剂热路线分别制备银纳米线。详细讨论了反应时间、反应气氛及反应物投料比等相关参数对银纳米线的产率和长径比的影响。发现密闭溶剂热法在缓解环境污染的同时降低了生长过程中的扰动,所得银纳米线平均直径约55 nm,长度约65μm,长径比接近1 200。以之制备的透明导电薄膜的方阻仅6Ω,波长550 nm下透光度为78. 6%,品质因数(FOM)高达246,优于常压滴注路线。     

A206/1%Al2O3铝基纳米复合材料的热裂行为

A206铝合金在金属型浇铸过程中具有高热裂倾向,难以用来制造重要铸件.采用超声分散法制备A206/1%Al2O3(质量分数,下同)纳米复合材料,在钢模中浇铸受限杆铸件来评价其热裂敏感性,利用光学显微镜(OM)和扫描电镜(SEM)对微观组织进行分析.结果表明:加入的A12O3纳米粒子在凝固过程中成为有效的异质形核核心,不仅使α-Al初晶从粗大枝晶转变为细小等轴晶,平均晶粒尺寸从164 μm降至26μm,而且在剩余液相中诱发形成大量富Fe,Mn的薄片状中间相,消除了粗大CuAl2相,从而显著降低了A206铝合金的热裂敏感性.     

纳米磁性金属电磁波吸收剂

分析了纳米磁性金属电磁波吸收剂的吸波原理,综述了纳米磁性金属电磁波吸收材料如零维磁性纳米颗粒、一维磁性金属纳米线、二维磁性薄膜、二维片状磁性金属颗粒的国内外研究进展情况,并对未来的研究方向提出见解。     

碳化温度对C/C复合材料微观结构及热性能的影响

采用CVI PIC工艺制备了四种碳毡增强碳基复合材料(C/C), 其中对三种样品A、B、C在2 500℃进行了一次石墨化处理,样品D未进行石墨化处理。为与900℃碳化对比,研究了1 500℃碳化对复合材料微观结构及热性能的影响。结果表明:碳化温度由900℃提高到1 500℃后,样品A的开孔率下降11. 6% ~13. 5%, 1 000℃的xy向线膨胀系数由1. 75×10-6 /K增大到2. 17×10-6 /K; xy向和z向的800℃热导率分别由65. 07W/(m·K)、45. 98W/(m·K)增大到75. 44W/(m·K)、54. 86W/(m·K);xy向和z向的比热容分别由1. 70kJ/(kg·K)、1. 43kJ/(kg·K)增大到1. 79kJ/(kg·K)、2. 19kJ/(kg·K)。样品B和样品C也表现出基本相同的趋势;随着碳化温度由900℃提高到1 500℃,样品D中微晶尺寸由2nm增大到4nm。     

核磁共振陀螺仪中三维磁场的初步锁定

核磁共振陀螺仪内部空间的三维磁场锁定作为关键技术之一,对于核磁共振陀螺仪的角度随机游走及零偏稳定性具有较大的优化作用。实验装置选用充有CS、^(129)Xe、^(131)Xe以及N_2的方形原子气室,选择895nm圆偏振光作为泵浦光,852nm线偏振光作为探测光,通过对纵向磁场进行调制,实现了三维原子磁力计。通过提升气室温度对纵向磁场的锁定效果进行优化后,在3个方向的磁场起伏范围均稳定至7nT(5000 s)以下,锁定后磁场的千秒稳定性比锁定前提升至少1个量级。     

泡沫碳化硅中碳化硅纳米线的原位生长及结构表征

利用蛋白质发泡法制备泡沫SiC陶瓷,以聚碳硅烷(PCS)为先驱体,采用化学气相沉积(CVD)工艺在泡沫SiC中原位生长出大量SiC纳米线。使用X射线衍射仪,扫描电子显微镜和透射电子显微镜对纳米线的物相组成和微观形貌进行表征。结果表明,纳米线直径为100～200nm,长度达到数百微米,均匀分布在泡沫SiC的气孔中,纳米线由沿1 1 1方向生长的β-SiC晶体组成,在纳米线顶端未发现球状催化剂存在,表明其生长机理主要为气-固(VS)生长机理。     

太阳风磁帆推进性能数值研究

利用考虑行星际磁场作用的磁流体动力学模型,建立了磁帆三维数值模拟方法,对计算方法的可靠性进行了验证,发现了线圈尾部的磁重联现象,研究了太阳风来流速度、等离子体离子数密度以及攻角对磁帆推进性能的影响。得出以下结论：不同速度、不同离子数密度的太阳风主要通过改变z方向电流的大小改变洛伦兹力,进而影响磁帆的推进性能：太阳风离子数密度恒定时,随着来流速度由30 km/s逐渐增大至75 km/s,z方向电流最大值由4 205 A/m²增至14 709 A/m²,磁帆所受推力由3.39 N增至13.40 N;太阳风来流速度恒定时,随着离子数密度由1.8×10¹⁹ m^-3增大至4.5×10¹⁹ m^-3,z方向电流最大值由6 039 A/m²增至10 585 A/m²,磁帆所受推力由6.62 N增至12.27 N。磁帆攻角变化,主要通过磁场构型的变化影响磁帆推进性能：攻角为0°和90°时的磁层半径分别为0.14 m和0.18 m,...     

几种新的单路原子磁导引磁场设计和分析

原子磁导引利用载流导线产生的磁场与原子相互作用来操控冷原子,针对冷原子操控和传输的要求,提出了双曲线薄板导引、双平行平板导引、三根等边三角形和四根正方形分布载流导线实现对冷原子进行单路磁导引的方案,利用Ansoft maxwell 2D软件计算各导引的磁场分布和沿特殊轴的磁场变化值,分析其导引特点。这几种磁导引都采用通直流电的载流导体,其结构中心位置的场强存在极小值,形成了沿着导引的方向呈现管状磁场分布,适合导引弱场搜寻态的原子。越接近导体表面的地方,磁场梯度越大,所以原子不易与材料的相互作用而被吸引到导体表面造成损耗,而且使用时不需另加控制磁场,在实验中易于实现。     

纳米化对电子束物理气相沉积制备Ni-20Cr-0．6Al合金氧化产物的影响

利用电子束物理气相沉积(EB-PVD)方法制备了厚度为0.5mm的N i-20Cr-0.6A l(wt%)合金薄板。合金的晶粒尺寸小于100nm。研究了N i-20Cr-0.6A l合金在1000℃空气中氧化100h后的氧化产物。结果表明,100h后在合金表面只生成了连续致密的-αA l2O3氧化膜。Cr含量为20%时,纳米化使生成连续A l2O3膜所需的最小铝含量大幅度下降。     

Effects of Different Molten-salt on the Synthesis of Hexagonal Barium Ferrite

Hexagonal-plate BaFe12O19 nano-particles were prepared by combining the co-precipitation and molten-salt method. The effects of molten-salt NaCl on the products have been compared with those of KCl. The X-ray diffraction analysis,the environment scanning electron microscopy and the vibrating sample magnetometer were used to measure their characteristics. The results show that the mol-ten-salt KCl is helpful to obtain pure phase while the molten-salt NaCl will prompt the crystallinity of particles to increase. It is also found that, given the molten-salt of NaCl and that of KCl of the same quantity, the particles formed are also the same size. The size of particles slightly increases as the quantity of the salt increases. Moreover, the sample prepared under 200% NaCl salt system has mag-netization of 71.5 emu/g.     

Effects of Different Molten-salt on the Synthesis of Hexagonal Barium Ferrite

Hexagonal-plate BaFe12O19 nano-particles were prepared by combining the co-precipitation and molten-salt method. The effects of molten-salt NaCl on the products have been compared with those of KCl. The X-ray diffraction analysis, the environment scanning electron microscopy and the vibrating sample magnetometer were used to measure their characteristics. The results show that the mol- ten-salt KCl is helpful to obtain pure phase while the molten-salt NaCl will prompt the crystallinity of particles to increase. It is also found that, given the molten-salt of NaCl and that of KCl of the same quantity, the particles formed are also the same size. The size of particles slightly increases as the quantity of the salt increases. Moreover, the sample prepared under 200% NaCl salt system has magnetization of 71.5 emu/g.     

多元掺杂对钡铁氧体吸波性能的影响

用柠檬酸溶胶凝胶法制备了Cu、Zr共掺钡铁氧体前驱体,研究煅烧温度对其物相的影响及Cu、Zr共掺对其吸波性能的影响。研究发现前驱体[BaFe11.2(Cu0.5Zr0.5)0.8O19]在1 200℃煅烧1 h,得到了单相的钡铁氧体。随着Cu、Zr掺量的增加,铁氧体的吸波性能提高。当Cu、Zr掺入量为0.8时,铁氧体的吸波性能最好,在10.4 GHz时,最大反射损耗达-7.81 dB。     

航空发动机整体叶盘磁力研磨光整实验

磁力研磨工艺抛光整体叶盘时,工件与磁极干涉严重,用径向磁极代替轴向磁极加工可有效避免干涉,但研磨压力小、研磨效率低.通过对磁力研磨径向磁极加工机理和单个研磨粒子的微观受力情况详细分析得到:提高磁场强度变化率可有效增大磁力研磨效率.经有限元模拟分析发现磁极表面沿轴线方向开矩形槽可使磁场强度变化率提高.对镍基高温合金材质整体叶盘进行磁力研磨实验,并对实验数据分析研究得出:以径向磁极为工具的磁力研磨法可实现对整体叶盘的无干涉加工,磁极开矩形槽后磁力研磨效率可提高31%,叶盘表面粗糙度值由研磨前的1.2μm降至0.18μm,验证了磁力研磨工艺对高效、高质量实现整体叶盘表面光整加工的可行性.      

人工槽模拟GH4169涡轮盘表面裂纹缺陷的微磁检测

针对航空发动机涡轮盘表面裂纹缺陷,提出一种地磁场环境下的微磁无损检测(NDT)方法。磁化试验测得了广泛使用的镍基高温合金GH4169材料的磁化特性曲线,通过磁性分析,证明该材料的相对磁导率略大于空气的相对磁导率,为弱顺磁性物质。理论分析了微磁检测适用于涡轮盘试件的检测原理和缺陷处的磁异常特征,通过对预置人工槽缺陷的涡轮盘试块进行检测,验证了理论分析的正确性。检测结果表明,随着涡轮盘表面裂纹宽度和深度的增加,磁异常的宽度和峰值也相应增加,裂纹宽度相同时,深度越深,或者说深宽比越大,磁异常越明显,且裂纹产生的位置对定位精度存在一定的影响。该微磁检测方法为涡轮盘表面裂纹缺陷的有效检测提供了新的思路,能进一步推广应用于飞机发动机的其他部件,如转子叶片、涡轮轴等,以及飞机机身上具有相似磁学特性的材料的无损检测。     

加速度计力矩器设计

介绍了永磁式力矩器的工作原理,对力矩器磁路计算进行了推导,介绍了提高磁性材料稳定性的方法,说明了力矩器磁温补偿的原理和方法.     

Auroral Plasma Acceleration Above Martian Magnetic Anomalies

Aurora is caused by the precipitation of energetic particles into a planetary atmosphere, the light intensity being roughly proportional to the precipitating particle energy flux. From auroral research in the terrestrial magnetosphere it is known that bright auroral displays, discrete aurora, result from an enhanced energy deposition caused by downward accelerated electrons. The process is commonly referred to as the auroral acceleration process. Discrete aurora is the visual manifestation of the structuring inherent in a highly magnetized plasma. A strong magnetic field limits the transverse (to the magnetic field) mobility of charged particles, effectively guiding the particle energy flux along magnetic field lines. The typical, slanted arc structure of the Earth’s discrete aurora not only visualizes the inclination of the Earth’s magnetic field, but also illustrates the confinement of the auroral acceleration process. The terrestrial magnetic field guides and confines the acceleration processes such that the preferred acceleration of particles is frequently along the magnetic field lines. Field-aligned plasma acceleration is therefore also the signature of strongly magnetized plasma. This paper discusses plasma acceleration characteristics in the night-side cavity of Mars. The acceleration is typical for strongly magnetized plasmas – field-aligned acceleration of ions and electrons. The observations map to regions at Mars of what appears to be sufficient magnetization to support magnetic field-aligned plasma acceleration – the localized crustal magnetizations at Mars (Acuña et al., 1999). Our findings are based on data from the ASPERA-3 experiment on ESA’s Mars Express, covering 57 orbits traversing the night-side/eclipse of Mars. There are indeed strong similarities between Mars and the Earth regarding the accelerated electron and ion distributions. Specifically acceleration above Mars near local midnight and acceleration above discrete aurora at the Earth – characterized by nearly monoenergetic downgoing electrons in conjunction with nearly monoenergetic upgoing ions. We describe a number of characteristic features in the accelerated plasma: The “inverted V” energy-time distribution, beam vs temperature distribution, altitude distribution, local time distribution and connection with magnetic anomalies. We also compute the electron energy flux and find that the energy flux is sufficient to cause weak to medium strong (up to several tens of kR 557.7 nm emissions) aurora at Mars. Monoenergetic counterstreaming accelerated ions and electrons is the signature of field-aligned electric currents and electric field acceleration. The topic is reasonably well understood in terrestrial magnetospheric physics, although some controversy still remains on details and the cause-effect relationships. We present a potential cause-effect relationship leading to auroral plasma acceleration in the nightside cavity of Mars – the downward acceleration of electrons supposedly manifesting itself as discrete aurora above Mars.     

基于磁极电流分配的电磁轴承控制器设计

 电磁轴承是机、电、磁一体化的复杂系统, 针对不对称、强耦合电磁轴承结构, 提出基于磁极电流分配的电磁轴承控制器设计。该方法将原来控制器分为反馈控制器和电流分配器两部分, 以简化控制器设计。主要讨论了轴承磁极电流分配器设计, 并应用于圆锥电磁轴承系统中, 设计它的磁极电流分配器。