纳米石墨薄片的制备、表征与应用

为了获得适宜于同聚合物进行纳米复合的纳米石墨薄片(NGS),采用微波膨化制备膨胀石墨(EG),利用超声剥离与表面修饰获得NGS,并借助SEM、XRD、FTIR等分析其微观结构。结果表明:EG由许多厚100-300 nm的石墨薄片连接而成并形成网络结构,孔隙尺寸约几十纳米到几十微米;通过对EG的超声剥离可破坏其原有网络结构并将石墨晶片进一步剥离为大量30-60 nm厚的石墨薄片;石墨微波膨化与超声剥离过程中微观形貌的变化及其表面活性基团的引入,有利于进一步借助插层法实现聚合物与石墨的纳米复合。     

纳米孔ZrO_2气凝胶的制备研究

以硝酸氧锆(ZrO(NO3)2.5H2O)为原料,采用水热法和超临界干燥技术制备了ZrO2气凝胶.利用SEM和BET等测试手段对所得气凝胶的结构和孔特征进行表征,分析了孔隙分布情况和孔结构.结果表明:气凝胶具有典型的纳米孔隙结构,孔径5＜Dp＜60nm,比表面积达916.5m2/g,孔分布均匀.对ZrO2凝胶过程进行了探讨.     

一维钡铁氧体纳米线的制备及操控

采用Sol-gel法,以自制的AAO模板制备了直径40～60nm,长度为150～200nm的一维BaFe12O19纳米线.利用X射线衍射(XRD),场发射扫描电镜(FESEM),振动样品磁强计(VSM)对BaFe12O19纳米线的组成、形貌与磁性能进行了研究.在外磁场的驱动下,对一维BaFe12O19纳米线进行操控.研究发现:BaFe12O19纳米线的易磁化方向平行其轴线方向,且操控后,BaFe12O19纳米线定向连接成“链”,当磁场与BaFe12O19纳米链阵列平行(∥)时,纳米链的剩余磁化强度(Mr)、饱和磁化强度(Ms)和最大磁能积(BH)m都得到增强.矫顽力(He)由3.98×105A/m增大至5.01×105 A/m,矩形比为0.9,可成为优异的高密度垂直磁记录材料.     

Deriving the Absolute Reflectance of Lunar Surface Using SELENE (Kaguya) Multiband Imager Data

The absolute reflectance of the Moon has long been debated because it has been suggested (Hillier et al. in Icarus 151:205–225, 1999) that there is a large discrepancy between the absolute reflectance of the Moon derived from Earth-based telescopic data and that derived from remote-sensing data which are calibrated using laboratory-measured reflectance spectra of Apollo 16 bulk soil 62231. Here we derive the absolute reflectance of the lunar surface using spectral data newly acquired by SELENE (Kaguya) Multiband Imager and Spectral Profiler. The results indicate that the reflectance of the Apollo 16 standard site, which has been widely used as an optical standard in previous Earth-based telescopic and remote-sensing observations derived by Multiband Imager, is 47% at 415 nm and 67% to 76% at 750 to 1550 nm of the value for the Apollo 16 mature soil measured in an Earth-based laboratory. The data also suggest that roughly 60% of the difference is caused by the difference in soil composition and/or maturity between the 62231 sampling site and the Apollo 16 standard site and that the remaining 40% difference can be explained by the difference between the compaction states of the laboratory and the actual lunar surface. Consideration of the compaction states of the surface soil demonstrates its importance for understanding the spectral characteristics of the lunar surface. We also explain and evaluate data analysis procedures to derive reflectance from Multiband Imager data.     

Extreme solar cycle variability in strong lines between 200 and 400 NM

Our study of solar cycle irradiance variability in the UV between 200 and 400 nm requires a detailed knowledge of the composition of the solar spectrum in this wavelength range. We compute the synthetic spectrum from 250 to 300 nm and compare it with ATLAS3 and SOLSTICE observations. Synthetic solar spectra for solar minimum and maximum conditions show large variations in broad, strong UV lines. Strong lines of FeI between 260 nm and 264 nm show increases between 0.4× and 3×in their max/min ratio. Our ``broad lines' database shows 167 lines with similar properties between 200 nm and 400 nm. Our results raise issues of the importance of such large variability in narrow bands and the difficulty of detection in measurements with spectral resolutions of 1 nm.     

机床振动对高精度金刚石刀具研磨质量的影响

研磨机床的振动是影响金刚石刀具机械研磨质量的重要因素,尤其在精密研磨工序。为了提高金刚石刀具的研磨质量,针对金刚石刀具的精密研磨工序,在研磨加工时对机床施加空气隔振垫,使研磨的金刚石刀具切削刃钝圆半径从隔振前的93.8nm降到了隔振后的72.7nm,前刀面表面粗糙度则从2.4nm降到了1.0nm,研磨质量得到明显改善。     

基于非线性双通MZI的多波长掺铒光纤激光器

提出了一种基于非线性双通MZI光纤滤波器的波长间隔可切换多波长掺铒光纤激光器.非线性双通MZI光纤滤波器除了多通滤波作用还具有功率均衡作用,能有效抑制掺铒光纤的增益竞争,从而实现室温下多波长稳定激射.通过合理调整激光腔内的偏振态,分别实现了0.2 nm和0.4 nm密集波长间隔可切换的多波长激光输出,两种状态下的激光波长个数分别为44个和25个,测量可得激光光信噪比分别高于14 dB和30dB.     

电荷作用对均质-非均质凝结流动的影响

基于Fletcher成核理论及均质-非均质凝结双流体模型,讨论了电荷作用对凝结流动的影响,结果表明:有无电荷影响时,成核率计算公式精度均较高,流场参数的计算结果与实验结果吻合良好,相对误差不超过5%,表明所建的均质-非均质凝结双流体模型具有较高精度.不带电时,加入颗粒半径为5nm颗粒前后流场过冷度差别较小,加入颗粒半径分别为8nm和10nm颗粒后过冷度峰值虽分别降低2K和7K,但均导致自发凝结向下游迁移.当颗粒带电荷量为Q=1e,加入颗粒半径为5nm颗粒情况下对减小成核自由能障、增加非均质成核率的作用最为明显,这一作用在颗粒半径为8nm时较弱,颗粒半径为10nm情况下最弱.当带电量增加至Q=3e时,加入颗粒半径分别为5nm和8nm颗粒情况下峰值过冷度与均质凝结相比分别下降10K和6K,且较明显地抑制了自发凝结发生.      

Galileo Ultraviolet Spectrometer experiment

The Galileo ultraviolet spectrometer experiment uses data obtained by the Ultraviolet Spectrometer (UVS) mounted on the pointed orbiter scan platform and from the Extreme Ultraviolet Spectrometer (EUVS) mounted on the spinning part of the orbiter with the field of view perpendicular to the spin axis. The UVS is a Ebert-Fastie design that covers the range 113–432 nm with a wavelength resolution of 0.7 nm below 190 and 1.3 nm at longer wavelengths. The UVS spatial resolution is 0.4 deg × 0.1 deg for illuminated disc observations and 1 deg × 0.1 deg for limb geometries. The EUVS is a Voyager design objective grating spectrometer, modified to cover the wavelength range from 54 to 128 nm with wavelength resolution 3.5 nm for extended sources and 1.5 nm for point sources and spatial resolution of 0.87 deg × 0.17 deg. The EUVS instrument will follow up on the many Voyager UVS discoveries, particularly the sulfur and oxygen ion emissions in the Io torus and molecular and atomic hydrogen auroral and airglow emissions from Jupiter. The UVS will obtain spectra of emission, absorption, and scattering features in the unexplored, by spacecraft, 170–432 nm wavelength region. The UVS and EUVS instruments will provide a powerful instrument complement to investigate volatile escape and surface composition of the Galilean satellites, the Io plasma torus, micro- and macro-properties of the Jupiter clouds, and the composition structure and evolution of the Jupiter upper atmosphere.     

激光增材制造技术常用金属材料激光吸收率测量

应用反射率测量装置对几种激光金属增材制造技术常用金属粉末和金属板材的激光吸收率进行间接测量。对比不同粒度、球形度金属粉末激光吸收率的大小;测量金属粉末和金属板材分别对1064nm红外激光和532nm绿光激光的吸收率大小。测量结果表明,粉末的球形度越好、粒径越大,粉末对激光吸收率越高;金属粉末和金属板材对1064nm激光的吸收率小于532nm激光的吸收率。测量结果可为这些金属材料的激光增材制造提供试验数据基础。     

Far ultraviolet imaging from the IMAGE spacecraft. 3. Spectral imaging of Lyman-α and OI 135.6 nm

Two FUV Spectral imaging instruments, the Spectrographic Imager (SI) and the Geocorona Photometer (GEO) provide IMAGE with simultaneous global maps of the hydrogen (121.8 nm) and oxygen 135.6 nm components of the terrestrial aurora and with observations of the three dimensional distribution of neutral hydrogen in the magnetosphere (121.6 nm). The SI is a novel instrument type, in which spectral separation and imaging functions are independent of each other. In this instrument, two-dimensional images are produced on two detectors, and the images are spectrally filtered by a spectrograph part of the instrument. One of the two detectors images the Doppler-shifted Lyman- while rejecting the geocoronal `cold Ly-, and another detector images the OI 135.6 nm emission. The spectrograph is an all-reflective Wadsworth configuration in which a grill arrangement is used to block most of the cold, un-Doppler-shifted geocoronal emission at 121.567 nm. The SI calibration established that the upper limit of transmission at cold geocoronal Ly- is less than 2%. The measured light collecting efficiency was 0.01 and 0.008 cm² at 121.8 and at 135.6 nm, respectively. This is consistent with the size of the input aperture, the optical transmission, and the photocathode efficiency. The expected sensitivity is 1.8×10^–2 and 1.3×10^–2 counts per Rayleigh per pixel for each 5 s viewing exposure per satellite revolution (120 s). The measured spatial resolution is better than the 128×128 pixel matrix over the 15°×15° field of view in both wavelength channels. The SI detectors are photon counting devices using the cross delay line principle. In each detector a triple stack microchannel plate (MCP) amplifies the photo-electronic charge which is then deposited on a specially configured anode array. The position of the photon event is measured by digitizing the time delay between the pulses detected at each end of the anode structures. This scheme is intrinsically faster than systems that use charge division and it has a further advantage that it saturates more gradually at high count rates. The geocoronal Ly- is measured by a three-channel photometer system (GEO) which is a separate instrument. Each photometer has a built in MgF₂ lens to restrict the field of view to one degree and a ceramic electron multiplier with a KBr photocathode. One of the tubes is pointing radially outward perpendicular to the axis of satellite rotation. The optic of the other two subtend 60° with the rotation axis. These instruments take data continuously at 3 samples per second and rely on the combination of satellite rotation and orbital motion to scan the hydrogen cloud surrounding the earth. The detective efficiencies (effective quantum efficiency including windows) of the three tubes at Ly- are between 6 and 10%.     

Photoluminescence Properties of Nanocrystalline 3C-SiC Films

Nanocrystalline (nc) 3C-SiC films on the Si substrate were prepared by the helicon wave plasma enhanced chemical vapor deposi-tion (HW-PECVD) technique. With the SiH4-CH4 gas flow ratio changing, the films exhibit different photoluminescence (PL) character-istics. Under the stoichiometric condition, the PL peak redshift from 470 nm to 515 nm is detected with the increase of excitation wave-length, which can be attributed to the quantum confinement effect radiation of 3C-SiC nanocrystals of different sizes. However, the ap-pearance of an additional PL band at 436 nm in Si-rich film might be sourced back to the excess of Si defect centers in it. This is also the case for C-rich film for its PL band lying at 570 nm. The results above quoted indicate an important influence of gas flow ratio on the PL properties of the SiC films providing an effective guidance for analyzing the luminescence mechanism and exploring the high-efficiency light emission of the SiC films.     

Comparison of Polar and Equatorial Coronal Holes Observed by UVCS/SOHO: Geometry and Physical Properties

We analyzed UVCS/SOHO data and compared the H I Lyα (121.6 nm) and O VI (103.2 nm, 103.7 nm) emission in the polar and equatorial coronal holes. We found that the emission lines have similar characteristics in these two types of coronal holes. Both types show evidence for superradially diverging boundaries. The latitudinal distribution of the O VI line ratio may indicate that the equatorial coronal hole has O⁺⁵ outflow velocities lower than in the polar coronal holes. This revised version was published online in June 2006 with corrections to the Cover Date.     

黏胶纤维在热解过程中微孔结构的演变

利用同步辐射X射线小角散射(SAXS)研究了黏胶基碳纤维原丝裂解过程中微孔的变化。结果表明:裂解过程中微孔沿轴向的半径由3.88砌逐渐增大到7.04nm,而垂直于轴向的半径则由3.86 nm减小至3.15 nm。因而,孔形由椭圆逐渐演变成针形,且取向趋向于纤维轴方向。分形研究表明:垂直于轴向的微孔分形雏数由2.40增大到2.61,而沿轴向的微孔分形维数则在2.00~2.23波动,说明随着裂解的进行,微孔结构逐渐趋于复杂化。微孔是影响纤维的力学性能主要因素,对纤维中的微孔结构的研究有着重要意义。     

背带式双波长全固态激光清洗设备

介绍了一种背带式18W全固态1064nm/532nm双波长激光清洗设备,其中,532nm绿光功率为6.4W,M2=2,不稳定度小于1%。针对表面油漆涂层和铁锈进行了清洗试验,并给出了清洗工件的金相图,结果表明能够满足工业清洗的要求。     

The Mercury Atmospheric and Surface Composition Spectrometer for the MESSENGER Mission

The Mercury Atmospheric and Surface Composition Spectrometer (MASCS) is one of seven science instruments onboard the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft en route to the planet Mercury. MASCS consists of a small Cassegrain telescope with 257-mm effective focal length and a 50-mm aperture that simultaneously feeds an UltraViolet and Visible Spectrometer (UVVS) and a Visible and InfraRed Spectrograph (VIRS). UVVS is a 125-mm focal length, scanning grating, Ebert-Fastie monochromator equipped with three photomultiplier tube detectors that cover far ultraviolet (115–180 nm), middle ultraviolet (160–320 nm), and visible (250–600 nm) wavelengths with an average 0.6-nm spectral resolution. It will measure altitude profiles of known species in order to determine the composition and structure of Mercury’s exosphere and its variability and will search for previously undetected exospheric species. VIRS is a 210-mm focal length, fixed concave grating spectrograph equipped with a beam splitter that simultaneously disperses the spectrum onto a 512-element silicon visible photodiode array (300–1050 nm) and a 256-element indium-gallium-arsenide infrared photodiode array 850–1,450 nm. It will obtain maps of surface reflectance spectra with a 5-nm resolution in the 300–1,450 nm wavelength range that will be used to investigate mineralogical composition on spatial scales of 5 km. UVVS will also observe the surface in the far and middle ultraviolet at a 10-km or smaller spatial scale. This paper summarizes the science rationale and measurement objectives for MASCS, discusses its detailed design and its calibration requirements, and briefly outlines observation strategies for its use during MESSENGER orbital operations around Mercury.     

纳米CeO2粉体的制备及其发光性能研究

以氨水和硝酸铈为反应原料,采用沉淀滴定法制备了纳米CeO2粉体,通过XRD、SEM、TEM等手段对其进行了结构表征和形貌分析;考察了不同溶剂、煅烧温度等对其颗粒尺寸的影响;应用荧光光谱法测试了其发光光谱,首次探讨了纳米CeO2粉体的发光性能。结果表明,前驱体经过300～700℃煅烧后可以得到颗粒尺寸为4-30nm的立方萤石结构CeO2晶体,其形貌接近于球形。在无水乙醇溶剂中得到的纳米CeO2颗粒分散较好,其颗粒尺寸随煅烧温度的升高而增大。纳米CeO2粉体具有良好的蓝光发光性能,在276nm的激发波长作用下,其发射光谱的最大峰值为473nm。     

变栅距光栅线位移传感器的温度影响分析

变栅距光栅线位移传感器工程样机完成后,进行了常态性能试验及环境试验,针对试验中出现的温度漂移问题,通过理论分析、试验验证、软件仿真,证实光栅组件的双金属片式翘曲为产生温漂问题的主要原因,并利用ANSYS-Workbench模拟得到解决方案,通过改进后的筒状腔体结构,使得温漂量值从12nm降到2nm以内.     

沉积含Si过渡层对于不锈钢上沉积的DLC薄膜的性能影响

本文介绍了采用RF-PECVD法在3Cr13不锈钢基体圆片上沉积制备类金刚石多层膜,其内层薄膜为掺Si的过渡层,外层为不同厚度的在50～1000 nm之间的类金刚石薄膜（DLC）。实验结果表明沉积过渡层可以有效提高薄膜与基体的结合力。类金刚石薄膜的摩擦系数和薄膜在摩擦过程中的损坏情况都与外层薄膜的厚度有关。     

相位偏移干涉测量中移相误差补偿技术研究

 在相位偏移干涉测量技术中,一阶线性和二阶非线性移相误差是产生相位检测误差的主要因素。在研究移相误差对相位偏移干涉法测量精度影响的基础上,提出五步移相算法一阶线性和二阶非线性移相误差补偿技术。该方法从相位偏移干涉图中拟和出移相过程中存在的移相误差,对五幅算法结果进行误差修正。试验证明移相器存在 10%一阶线性误差和 1 %二阶非线性误差时,五幅算法相位检测误差为 0.12弧度;采用该补偿方法可以将相位测量精度减少到 0.02弧度,相当于采用氦氖激光器的倍程干涉仪中位移测量精度从 6.0 nm提高到 1 nm。