氧化镍电致变色薄膜及其器件的制备与性能研究

以氧化铟锡（ITO）玻璃为基底，采用直流反应磁控溅射法在室温环境下制备了高透过率调制的NiO_x薄膜，利用X射线衍射仪（XRD）、扫描电子电镜 （SEM）、紫外可见分光光度计（UV 3600）对薄膜进行分析和表征，研究溅射过程中氩氧比、气压、功率对薄膜结构、形貌及电致变色性能的影响。结果表明：制备的NiO_x薄膜表面有明显的结晶颗粒及孔隙，并沿（200）晶面择优生长；随着气压、功率、氧分压的增大，透过率调制先增大后减小，在时间为45 min、溅射气压4.9 Pa、氩氧比113∶7、功率215 W时最高可达58.3%，着褪色响应时间分别为9和19 s，相应的着褪色效率分别为77.56和40.39 cm²/C；以最优工艺的NiO_x薄膜组装了结构为Glass/ITO/NiO_x/Li-electrolyte/WO₃/ITO/Glass的电致变色器件，器件在550 nm处的光调制幅度为46.5%，着褪色时间分别为27和45 s，相应的着褪色速率为1.5和0.9 %/s，在循环500次后透过率调制保持在40%以上。     

具有纳米结构的 VO_2 相变薄膜

采用无机溶胶－凝胶法制备ＶＯ２相变薄膜，该薄膜相变时的电阻（率）突变可达４～５个数量级。并用ＸＲＤ，ＤＳＣ和ＴＧＡ法研究了制膜过程中干凝胶膜的层状非晶纳米结构。通过适当的非晶晶化过程及随后Ｖ２Ｏ５→ＶＯ２转变的真空热处理，可获得带有空洞（ｖｏｉｄ）结构的低密度纳米薄膜，从而使电阻（率）突变特性异常优异     

不同钝化工艺SiO2薄膜的辐射缺陷

为研究不同钝化工艺栅介质用SiO₂薄膜的高能电子辐射缺陷特征，采用能量为1 MeV的高能电子在辐照注量为1×10¹⁵ e/cm²、5×10¹⁵ e/cm²和1×10¹⁶e/cm²下对三种不同钝化工艺（I，700 nm SiN + 500 nm PSG;II，1.2 μm SiN;III，700 nm PSG + 500 nm SiN）的SiO₂薄膜进行了辐照试验。拉曼光谱和X射线光电子能谱结果表明I和III钝化工艺SiO₂薄膜形成了非晶硅及双氧根离子，傅立叶红外光谱结果表明I钝化工艺SiO₂薄膜形成缺陷结构未知的A₁、A₂、B₁及B₂缺陷；II钝化工艺SiO₂薄膜形成A₁、B₁、及 缺陷；III钝化工艺SiO₂薄膜形成A₁、及B₂缺陷。     

g-C3N4/Fe2O3复合催化剂的表征及其对AP的催化作用

为了改善固体推进剂中高氯酸铵（AP）热分解性能,降低其热分解温度,利用SEM,XRD,FT-IR对原位制备的g-C₃N₄/Fe₂O₃复合催化剂的形貌和结构进行了表征,通过差示扫描量热法（DSC）考察了催化剂对AP 热分解的催化效果。结果表明：g-C₃N₄/Fe₂O₃复合结构完整,Fe₂O₃颗粒紧密负载在g-C₃N₄上;加入不同质量分数的复合催化剂,AP的低温分解峰和高温分解峰都明显降低,且随着催化剂加入量的增加催化效果增强;加入复合催化剂质量分数5%时,高温分解峰和低温分解峰分别降低到348.1℃和281.7℃,表明g-C₃N₄/Fe₂O₃复合催化剂可有效降低AP的热分解温度,改善其热分解性能。     

引入TaSi2对ZrB2-20%SiC抗氧化性能的影响

将TaSi₂引入到ZrB₂-20%SiC中得到ZrB₂-10%SiC-10%TaSi₂，并在1 000、1 200、1 500和1 650℃有氧条件下分别氧化5、15和30 min。复合材料通过热压烧结法制备（1 950℃/30 MPa/30 min），并通过XRD及SEM等方法对氧化后的质量变化及微观结构进行了分析。结果表明，TaSi₂的引入提高了ZrB₂-20%SiC的致密度和力学性能，但是在1 200℃以上温度氧化时，ZrB₂-10%SiC-10%TaSi₂的抗氧化性有所降低。     

利用遗传算法和LMI设计固定结构H2/H∞飞行控制律

 在设计飞翼式无人机(UAV)的横航向飞行控制系统时,为了使无人机具有较好的动态特性和阵风抑制能力,同时又便于工程实现,提出了固定结构的H₂/H_∞控制律设计方法。对于由此遇到的双线性矩阵不等式(BMI)问题,先用线性矩阵不等式(LMI)方法得到控制律参数和H₂/H_∞性能指标的映射关系,再用此映射关系作为适应度函数,用改进的遗传算法求解使H₂/H_∞性能最优的控制律参数。仿真结果表明,使用固定结构的H₂/H_∞控制方法的无人机动态响应迅速平滑,在侧风干扰下的滚转角振荡幅值仅是原经典控制方法的一半。     

基于LMI的航空发动机鲁棒H_∞控制器设计

 研究了系统矩阵均具有参数不确定性系统的非标准H_∞鲁棒控制问题。基于 LMI的H_∞控制器设计方法,给出了参数不确定性系统用 3个线性矩阵不等式表征的非标准H_∞控制问题可解的充分必要条件,采用“内点法”求解线性矩阵不等式,可得使闭环系统对于所有可能的参数不确定性均二次稳定且传递函数的H∞ 范数 γ有界的鲁棒控制解。该方法应用于非“标准”系统——某型双转子涡喷发动机稳态双变量调节控制器的设计,通过在气动热力学模型上的仿真结果表明,取得了良好的结果。     

等离子喷涂LaTi2Al9O19热障涂层的微观组织结构及热物理性能

 第一代热障涂层(TBCs)由氧化钇部分稳定的氧化锆(YSZ)陶瓷隔热层和金属粘结层组成,该涂层长期使用温度低于1 200℃。随着先进航空发动机向着高推重比发展,迫切要求发展新一代超高温、高隔热热障涂层材料。LaTi₂Al₉O₁₉(LTA)在1 500℃长期保持相稳定,是一种非常有前景的超高温热障涂层候选材料。本文采用大气等离子喷涂(APS)制备了LTA涂层,研究了喷涂工艺对涂层微观组织结构和热物理性能的影响。结果表明沉积态涂层中含少量的非晶态,在860℃和1 130℃出现晶化峰。等离子喷涂过程中La₂O₃挥发量较多,导致沉积态涂层中La元素与原始粉末相比含量偏低,而其他组分的化学成分随喷涂功率变化不大。LTA涂层的热扩散系数在1 400℃下为0.3~0.4 mm²·s^-1,热导率为1.1~1.6 W·m^-1·K^-1。1 050℃经过20小时热处理后,得到晶化的涂层在晶化温度范围内的热扩散系数和热导率值均增大。随着喷涂功率减小,涂层孔隙率增加,热导率减小。     

共沉淀法制备花状NiCo2O4及其吸波性能的研究

通过共沉淀法制备花状NiCo₂O₄吸波材料，利用XRD、FTIR、BET、XPS和SEM等方式表征了样品成分及形貌特征，将不同煅烧温度（300、400、500、600、700 ℃）的产物利用矢量网络分析仪通过同轴测试法模拟了不同厚度下的吸波性能。结果表明：400 ℃煅烧样品在反射损耗值、吸收带宽以及样品厚度都表现出较好的性能，当厚度为1.5 mm时，在14.32 GHz处吸波材料达到最大的吸收损耗值为-43.71 dB，有效吸收带宽为4.48 GHz （12.08~16.56 GHz），可以预见镍钴基吸波材料具有很大的潜力。     

Al2O3/ZrO2(n)微纳米复合陶瓷超声振动精密磨削表面微观特征试验研究

 基于Al₂O₃/ZrO₂（n）微纳米复合陶瓷的“晶内型”微观结构，应用原子力显微镜(AFM)重点分析了微 纳米复合陶瓷二维超声振动磨削表面微观形貌。结合磨削表面X射线衍射定性分析与定量计算，研究了“晶内型”微纳米复合陶瓷材料超精密振动磨削表面变质层结构。X射线衍射分析表明：二维振动磨削和普通磨削表面均以α-Al₂O₃和四方相ZrO₂为主，存在少量单斜相ZrO₂，磨削表面无非晶相产生；磨削表层和基体之间的过渡层的X射线衍射峰具有半峰宽化现象。AFM分析结果表明：细粒度金刚石砂轮普通磨削和振动磨削表面均无微裂纹和断裂破碎，磨削表面粗糙度是由不同幅值的多种波形叠加的结果；AFM轮廓特征分析表明：二维超声振动磨削表面峰谷较均匀，磨削表面均匀一致性优于普通磨削表面；材料晶化过程中产生的固有缺陷是限制硬脆材料近纳米表面形成的重要因素。     

Fe-Cr-Al/Si非晶态薄膜的电阻-应力特性

 对非晶态Fe-Cr-Al/Si薄膜研究了方块电阻与灵敏度、电阻温度系数、电阻率以及薄膜厚度等的关系;根据升温时薄膜电阻开始剧变推算了薄膜的晶化温度,并评估了Fe-Cr-Al/Si薄膜作为力传感器敏感材料的品质。     

The Student Dust Counter on the New Horizons Mission

The Student Dust Counter (SDC) experiment of the New Horizons Mission is an impact dust detector to map the spatial and size distribution of dust along the trajectory of the spacecraft across the solar system. The sensors are thin, permanently polarized polyvinylidene fluoride (PVDF) plastic films that generate an electrical signal when dust particles penetrate their surface. SDC is capable of detecting particles with masses m>10^?12 g, and it has a total sensitive surface area of about 0.1 m², pointing most of the time close to the ram direction of the spacecraft. SDC is part of the Education and Public Outreach (EPO) effort of this mission. The instrument was designed, built, tested, integrated, and now is operated by students.     

离子束辅助沉积WS_2-Ti-Ag复合薄膜的摩擦性能

采用ZDH-100型号离子束复合沉积设备沉积WS_2-Ti-Ag复合薄膜,基材为轴承钢和单晶硅(100).采用场发射扫描电子显微镜、XRD衍射仪,检测复合薄膜的表面形貌、微观结构.采用球-盘式摩擦磨损试验机,对复合薄膜在大气环境中的摩擦性能进行了研究.结果表明:采用离子束辅助沉积技术制备的WS_2-Ti-Ag复合薄膜是非晶态薄膜;并且随法向载荷的增加,复合薄膜的摩擦因数减小,摩擦状态越稳定,耐磨寿命越短.     

Emergence of a Habitable Planet

We address the first several hundred million years of Earth’s history. The Moon-forming impact left Earth enveloped in a hot silicate atmosphere that cooled and condensed over ∼1,000 yrs. As it cooled the Earth degassed its volatiles into the atmosphere. It took another ∼2 Myrs for the magma ocean to freeze at the surface. The cooling rate was determined by atmospheric thermal blanketing. Tidal heating by the new Moon was a major energy source to the magma ocean. After the mantle solidified geothermal heat became climatologically insignificant, which allowed the steam atmosphere to condense, and left behind a ∼100 bar, ∼500 K CO₂ atmosphere. Thereafter cooling was governed by how quickly CO₂ was removed from the atmosphere. If subduction were efficient this could have taken as little as 10 million years. In this case the faint young Sun suggests that a lifeless Earth should have been cold and its oceans white with ice. But if carbonate subduction were inefficient the CO₂ would have mostly stayed in the atmosphere, which would have kept the surface near ∼500 K for many tens of millions of years. Hydrous minerals are harder to subduct than carbonates and there is a good chance that the Hadean mantle was dry. Hadean heat flow was locally high enough to ensure that any ice cover would have been thin (<5 m) in places. Moreover hundreds or thousands of asteroid impacts would have been big enough to melt the ice triggering brief impact summers. We suggest that plate tectonics as it works now was inadequate to handle typical Hadean heat flows of 0.2–0.5 W/m². In its place we hypothesize a convecting mantle capped by a ∼100 km deep basaltic mush that was relatively permeable to heat flow. Recycling and distillation of hydrous basalts produced granitic rocks very early, which is consistent with preserved >4 Ga detrital zircons. If carbonates in oceanic crust subducted as quickly as they formed, Earth could have been habitable as early as 10–20 Myrs after the Moon-forming impact.     

Numerical Simulations of the Warm-Hot Intergalactic Medium

In this paper we review the current predictions of numerical simulations for the origin and observability of the warm hot intergalactic medium (WHIM), the diffuse gas that contains up to 50 per cent of the baryons at z∼0. During structure formation, gravitational accretion shocks emerging from collapsing regions gradually heat the intergalactic medium (IGM) to temperatures in the range T∼10⁵–10⁷ K. The WHIM is predicted to radiate most of its energy in the ultraviolet (UV) and X-ray bands and to contribute a significant fraction of the soft X-ray background emission. While O vi and C iv absorption systems arising in the cooler fraction of the WHIM with T∼10⁵–10^5.5 K are seen in FUSE and Hubble Space Telescope observations, models agree that current X-ray telescopes such as Chandra and XMM-Newton do not have enough sensitivity to detect the hotter WHIM. However, future missions such as Constellation-X and XEUS might be able to detect both emission lines and absorption systems from highly ionised atoms such as O vii, O viii and Fe xvii.     

光学滤光片薄膜边缘应力研究

以光学滤光片薄膜边缘应力作为对象,研究了Ge/Zn S单、多层光学薄膜应力的变化规律。通过实验研究了离子束轰击能量以及真空退火温度等因素对Ge/Zn S光学薄膜应力类型、大小、变化及其分布的影响规律。Zn S薄膜的应力为压应力,采用离子束辅助工艺后薄膜边缘应力变得均匀;真空退火使Zn S薄膜的应力减小为原来的一半。通过优化沉积参数和张应力、压应力薄膜的组合降低了Ge/Zn S多层光学薄膜的应力,结果表明其平均应力分别为0.1 MPa,而且处于压应力状态。     

Study of Dynamic Loads of Aircraft Bevel Gear Systems

This paper studies the dynamic loads of bevel gears with circular and straight teeth with the overlap factors less than two (ε_α < 2) and more than two (ε_α > 2). The advantages of the gears with straight teeth with ε_α > 2 are shown.     

Singular formalism and admissible control of spacecraft with rotating flexible solar array

This paper is concerned with the attitude control of a three-axis-stabilized spacecraft which consists of a central rigid body and a flexible sun-tracking solar array driven by a solar array drive assembly. Based on the linearization of the dynamics of the spacecraft and the modal identi- ties about the flexible and rigid coupling matrices, the spacecraft attitude dynamics is reduced to a formally singular system with periodically varying parameters, which is quite different from a space- craft with fixed appendages. In the framework of the singular control theory, the regularity and impulse-freeness of the singular system is analyzed and then admissible attitude controllers are designed by Lyapunov＇s method. To improve the robustness against system uncertainties, an H∞ optimal control is designed by optimizing the H∞ norm of the system transfer function matrix. Comparative numerical experiments are performed to verify the theoretical results.     

An Update on Ultra-Heavy Elements in Solar Energetic Particles above 10 MeV/Nucleon

Measurements below several MeV/nucleon from Wind/LEMT and ACE/ULEIS show that elements heavier than Zn (Z=30) can be enhanced by factors of ∼100 to 1000, depending on species, in ³He-rich solar energetic particle (SEP) events. Using the Solar Isotope Spectrometer (SIS) on ACE we find that even large SEP (LSEP) shock-accelerated events at energies from ∼10 to >100 MeV/nucleon are often very iron rich and might contain admixtures of flare seed material. Studies of ultra-heavy (UH) SEPs (with Z>30) above 10 MeV/nucleon can be used to test models of acceleration and abundance enhancements in both LSEP and ³He-rich events. We find that the long-term average composition for elements from Z=30 to 40 is similar to standard solar system values, but there is considerable event-to-event variability. Although most of the UH fluence arrives during LSEP events, UH abundances are relatively more enhanced in ³He-rich events, with the (34<Z<40)/O ratio on average more than 50 times higher in ³He-rich events than in LSEP events. At energies >10 MeV/nucleon, the most extreme event in terms of UH composition detected so far took place on 23 July 2004 and had a (34<Z<40)/O enhancement of ∼250–300 times the standard solar value.