金合金锡铅软钎焊接头脆性行为

采用Sn63Pb37钎料对Au60AgCu合金进行钎焊试验.对钎焊接头的微观组织、显微硬度、化合物相成分、力学性能及断口形貌进行了分析,并探讨了界面化合物相对接头脆性的影响.结果表明:Au60AgCu合金接头化合物主要由AuSn₂,AuSn₄和Ag₃Sn组成.金属间化合物的硬度很高,其厚度随钎焊温度的升高及保温时间的增长而增厚.钎焊接头剪切性能测试表明,断裂发生在金属间化合物层,断口形貌为脆性断裂.     

CeO2纳米粒子的自组装结构合成、表征及催化特性

利用微乳液方法(以AOT为表面活性剂)自组装合成了叶脉状结构的CeO₂(氧化铈)纳米粒子;使用X射线衍射仪(XRD)、透射电子显微镜(TEM)、括展X射线精细结构(EXAFS)对其进行了研究表征;并对其催化特性进行了测试. XRD结果表明CeO₂纳米粒子为立方面心结构;EXAFS结果表明与体相CeO₂微粒相比,Ce－O键长变长,Ce原子周围O原子配位数降低;催化特性研究结果表明,相对于体相材料,CeO₂纳米微粒的催化分解H₂O₂的活性大大提高.     

钛合金的离子束改性

钛合金是航空航天工业常用的结构材料,它具有重量轻、强度高、抗腐蚀强等优良性能,但耐磨性较差.为提高其耐磨性,对TC4、TA7航材试件,采用溅射方法在其表面镀上钛膜,并用(N^＋＋N^＋₂)混合离子束进行动态反冲注入及单元素C^＋离子束注入两种方法,进行表面改性.精密摩擦、磨损试验及显微硬度测量结果,试件表面的滑动摩擦系数降低了64%~77%;磨损率减少了22%~48%;显微硬度提高0.3~1.4倍.证明离子注入有效地改善了合金表层的摩擦、磨损性能.对注入样品进行X射线光电子能谱(XPS)分析,发现注入后的钛合金表层,生成了大量的TiO₂,并析出TiN,TiC等金属化合物,这是降低摩擦系数,提高耐磨性的主要因素.添加C^＋离子注入的试件,其力学性能并无进一步改善,原因有待分析.     

LSTM神经网络在太阳F10.7射电流量中期预报中的应用

F_10.7指数作为大气密度经验模型的重要输入参量，其预报精度直接影响航天器轨道预报精度.研究发现，太阳活动表现出长时间尺度上平均11年和中短时间尺度平均27天的周期性变化特征.依据这一观测事实，基于长短期记忆单元（Long Short-term Memory，LSTM）递归神经网络方法进行F_10.7指数未来27天的中期预报.利用一个连续长时段F_10.7数据作为训练数据，构建LSTM神经网络训练和预测模型，分别预测太阳活动高低年未来27天的F_10.7指数.结果表明，太阳活动高年的第27天F_10.7指数预报平均相对误差最优可达10%以内，低年最优可达2%以内.      

L10结构金属间化合物空位形成能

L1₀结构CoPt和FePt 薄膜因其高磁各向异性而成为新一代超高磁记录密度材料.采用Miedema理论计算了多种L1₀结构金属间化合物的空位形成能.研究结果表明:在这些金属间化合物中可能形成的空位类型,如FeNi和MnNi合金中易形成Ni空位;FePt和FePd合金中易形成Fe空位;CoPt合金中易形成Co空位;NiPt合金中易形成Ni空位;MnPt合金中易形成Pt空位;MnPd和MnHg合金中易形成Mn空位;MnRh合金中易形成Rh空位.这一研究结果为进一步研究开发高性能的磁性薄膜提供了理论依据.     

铝合金阳极化膜上铈转化膜沉积的电化学研究

阳极氧化膜在含1g/L CeCl₃和2.7 g/L H₂O₂的水溶液中阴极电解可以在其表面沉积富铈转化膜.用循环伏安、φ-t和j-t曲线等电化学测试方法对转化膜成膜反应进行了研究,以期获得对成膜机理的深入了解和证实根据其它工作提出的成膜机理.研究结果表明铈转化膜的生成包括阳极氧化膜的化学溶解和4价铈化合物的电化学还原两个过程;在阴极电位达到析氢电位之前,这两个过程主要是由H₂O₂在阴极的电还原改变了阴极表面附近溶液的局部pH值引起的,而O₂的还原通常不能引起这两个过程的发生.      

激光快速熔凝Al2O3/YAG共晶陶瓷的制备与组织

采用激光快速熔凝技术制备Al₂O₃/YAG共晶自生复合陶瓷, 研究Al₂O₃/YAG共晶陶瓷在高能激光束作用下,不同扫描速率(0.01~2.0mm/s)、超高温度梯度下的凝固组织特征及其生长机制,探索激光熔凝过程控制参数与凝固组织的关系.研究结果表明:激光熔凝Al₂O₃/YAG共晶陶瓷由无规则连续分布的Al₂O₃相和YAG相两相组成,没有晶界和其他相,Al₂O₃相的体积分数为(45.0±2.0)%,两相耦合生长,交错分布,是典型的快速凝固层片状非规则共晶组织;共晶层间距细密, 并随激光扫描速度的增大而减小,扫描速度为0.02mm/s 时,共晶间距约为1~2μm,扫描速度为2.0mm/s时,共晶间距仅为0.5μm左右;综合热分析表明,Al₂O₃/YAG共晶熔点为2096K,与相图吻合.     

离心力场中TiC/FeNiCr复合材料 涂层的原位反应合成

以Fe₂O₃,Cr₂O₃,CrO₃,NiO,Al,Ti粉和C粉为原料,在离心力场中在碳钢基体表面原位反应合成了TiC-FeNiCr复合材料涂层.利用X射线衍射、金相照相、扫描电镜、X射线能谱分析等手段对涂层的显微结构和组织形貌进行了研究.测试了涂层的显微硬度及干滑动磨损条件下的耐磨性能.结果表明,涂层和碳钢基体能形成冶金结合.涂层由FeNiCr奥氏体和其中弥散分布的TiC硬质相组成.TiC颗粒晶粒尺寸小于3μm,形状呈多边形或花瓣状.涂层显微硬度约为Hv 500~Hv 800,TiC含量增加,涂层的显微硬度提高.涂层较碳钢具有优异的耐磨性能.      

LD30铝合金与304不锈钢低温钎焊润湿性研究

采用LD30铝合金与304不锈钢低温钎焊工艺进行润湿性研究。通过润湿性研究对比,选用了60Sn-40Pb、Sn-3.5Ag和35Sn-40Pb-25Bi3种 适用于LD30铝合金和304不锈钢的低熔点钎料,并针对每种钎料选取与之相匹配的钎剂。分析了接头的微观组织、化合物相成分和X射线探伤。结果表明:60Sn-40Pb 和35Sn-40Pb-25Bi与H₃PO₄组合在304不锈钢上润湿性很好;不锈钢与镀镍层铝合金钎焊试验时,60Sn-40Pb和35Sn-40Pb-25Bi与50% H₃PO₄+50%乙二醇组合润湿性很好;Sn-3.5Ag 钎料润湿性相对较差。      

热冲击作用下钨钒合金的表面开裂及熔化行为

本文研究了机械合金化+热压（HP）烧结制备的钨钒（W-V）合金在热冲击作用下的表面损伤行为。以合金中钒的质量分数作为变量,探究钒质量分数的变化（1%~10%）对钨钒合金抗热冲击性能的影响。利用光学显微镜、扫描电镜、能谱仪、纳米压痕仪等多种测试方式,分析表征了HP烧结钨钒合金的组织结构特征及其经过热冲击测试后的表面开裂及熔化行为特征。结果表明:在1 800℃、20 MPa的压力条件下保温2 h可以制备出致密度高、合金化程度高的钨钒合金,且随着钒质量分数的增加,合金样品的致密度有所提高;合金样品中钨基体硬度大于富钒相,在高能电子束模拟的国际热核聚变实验堆（ITER）边界局域模（ELMs）热冲击作用下,钨基体对裂纹扩展的阻碍作用明显强于富钒相;随着钒质量分数的升高,合金的开裂阈值和熔化阈值均降低,本文对相关机理进行了讨论。      

Implementation of a new characteristic parameter into the IRI sub-peak electron density profile

The shape of electron density profile in the International Reference Ionosphere could be improved significantly if the height h_g and electron density N_g of the F region sub-peak inflexion point were entered in the set of the profile standard parameters. To study variations of these important parameters, the N(h) analysis of the statistically-summarized ionograms at the latitudes of 40–80°N of the Eastern hemisphere has been carried out for the two-hours intervals of local time, three seasons (winter, equinox and summer) and two levels of solar activities characterized by Covington indicesF_10.7 = 100 and 200. It is shown that the parameters of the inflexion point can be expressed in most cases via the peak parameters of the F2 layer ash_g= 0.8 hmF2 and N_g= 0.5 NmF2.     

顺电相PbTiO3晶体的电子结构和光学性质

应用全电势线形平面波缀加方法对铁电晶体钛酸铅的顺电立方相的电子能带结构、态密度、电子密度分布进行了计算.能带结构的计算结果表明立方顺电相晶体PbTiO₃为直接带隙的半导体,带隙大小为1.7eV.通过态密度和电子密度的计算结果分析,得到价带和导带的电子组成情况,并且指出Ti原子和O原子存在较强的共价键合.在电子结构的计算基础上,计算得到了与实验符合较好的PbTiO₃晶体的介电函数的实部和虚部,分析了虚部所对应的能带跃迁,并得到了其它的光学性质的参数(光学吸收系数、折射率、消光系数、能量损失曲线、反射率).     

硼酸金属化合物的制备及其电催化活性

采用电化学沉积法于室温、碱性条件下在氧化铟锡(ITO,Indium Tin Oxide)表面制备了硼酸钴(CoBi)、硼酸镍(NiBi)、硼酸锰(MnBi)、硼酸铑(RhBi)、硼酸钯(PdBi)几种无定形的硼酸金属化合物薄膜,并对其形貌和结构进行表征,结果表明几种薄膜均为无定形结构.将这几种硼酸金属化合物应用于电化学催化水氧化制氧,对比其催化活性,发现CoBi,NiBi,RhBi具有较高的催化性能,而MnBi和PdBi催化活性较低.进一步研究硼酸pH值对CoBi电催化水分解的影响.发现硼酸有利于金属化合物的制备,pH7~11范围内,HBO₃^2-作为质子受体含量逐渐增大,能接受放氧过程产生的质子,促进催化水分解过程的进行.所得催化剂可自我修复,实现循环利用.     

Sensitivity on nonequilibrium chemical systems to gravitational field

We note that far-from-equilibrium chemical systems can respond very sensitively to gravity. The response could be in selection of possible structures or in the formation of propagating bands. In these cases the sensitivity is characterized by the factor $\text{(E}{}_{\mathrm{g}}\text{/kT)}{}^{\mathrm{<mtext>1</mtext><mtext>n</mtext>}}$, where n=2 or 3, E_g the interaction energy, k the Boltzmann constant and T, the temperature. Also, taking the thermodynamic fluctuations into account, we obtain the theoretical limit for the minimum field strength measurable by such systems.     

Multiple wavelength observations of flaring active regions

We present observations of flaring active regions with the Very Large Array (V.L.A. at 6 cm and 20 cm wavelengths) and the Westerbork Synthesis Radio Telescope (W.S.R.T. at 6 cm wavelength). These are compared with photospheric magnetograms (Meudon) and with Hα and offband Hα photographs (Big Bear and Ottawa River Solar Observatories). The 6 cm radiation of these active regions marks the legs of dipolar loops which have their footpoints in lower-lying sunspots. The intense, million degree radiation at 6 cm lies above sunspot umbrae in coronal regions where the longitudinal magnetic field strength H_? = 600 Gauss and the height above the sunspot umbrae h = 3.5±0.5 × 10⁹ cm. Circularly polarized horseshoe structures at 6 cm ring the sunspot umbrae. The high degree of circular polarization (?_c = 95%) of the horseshoes is attributed to gyroresonant emission above sunspot^? penumbrae. The 20 cm radiation of these active regions exhibits looplike coronal structures which extend across regions of opposite magnetic polarity in the underlying photosphere. The 20 cm loops are the radio wavelength counterparts of the X-ray coronal loops. We infer semilengths L = 5 × 10⁹ cm, maximum electron temperatures T_e(max) = 3 × 10⁶ K, emission measures ∫N_e²d$\text{l}$ = 10²⁸ cm^?5, and electron densities N_e = 10⁹ cm^?3 (or pressures p = 1 dyn cm^?2) for the 20 cm bremsstrahlung. A total of eight solar bursts were observed at 6 cm or 20 cm wavelength with second-of-arc angular resolution. The regions of burst energy were all resolved with angular sizes between 5″ and 30″, brightness temperatures between 2 × 10⁷ K and 2 × 10⁸ K, and degrees of circular polarization between 10% and 90%. The impulsive phase of the radio bursts are located near the magnetic neutral lines of the active regions, and between the flaring Hα kernels which mark the footpoints of magnetic loops. In one case there was preburst heating in the coronal loop in which a burst occurred. Snapshot maps at 10 s intervals reveal interesting burst evolution including rapid changes of circular polarization and an impulsive burst which was physically separated from both the preburst radio emission and the gradual decay phase of the burst.     

等离子喷涂纳米TiO2涂层及其光催化性能

原始喷涂粉末经过喷雾干燥法造粒,采用等离子喷涂工艺在普通载玻片上制备了纳米TiO₂涂层,并对涂层在300℃,400℃,500℃进行热处理.采用X射线衍射(XRD)方法对TiO₂涂层进行了相结构分析;用扫描电子显微镜(SEM)、透射电子显微镜(TEM)观察涂层的微观形貌;用压汞方法测量涂层的孔隙率.结果表明,喷涂后锐钛矿型TiO₂含量大约在30%~50%,粒径10~30nm,孔隙率小于6%,热处理后涂层更致密,孔隙率降低.喷涂电流为400A且未经过热处理的TiO₂涂层具有最佳光催化效果.     

Bottom side profiles for two close stations at the southern crest of the EIA: Differences and comparison with IRI-2012 and NeQuick2 for low and high solar activity

Bottom side electron density profiles for two stations at the southern crest of the Equatorial Ionization Anomaly (EIA), São José dos Campos (23.1°S, 314.5°E, dip latitude 19.8°S; Brazil) and Tucumán (26.9°S, 294.6°E, dip latitude 14.0°S; Argentina), located at similar latitude and separated by only 20° in longitude, have been compared during equinoctial, winter and summer months under low (year 2008, minimum of the solar cycle 23/24) and high solar activity (years 2013–2014, maximum of the solar cycle 24) conditions. An analysis of parameters describing the bottom side part of the electron density profile, namely the peak electron density NmF2, the height hmF2 at which it is reached, the thickness parameter B₀ and the shape parameter B₁, is carried out. Further, a comparison of bottom side profiles and F-layer parameters with the corresponding outputs of IRI-2012 and NeQuick2 models is also reported. The variations of NmF2 at both stations reveal the absence of semi-annual anomaly for low solar activity (LSA), evidencing the anomalous activity of the last solar minimum, while those related to hmF2 show an uplift of the ionosphere for high solar activity (HSA). As expected, the EIA is particularly visible at both stations during equinox for HSA, when its strength is at maximum in the South American sector. Despite the similar latitude of the two stations upon the southern crest of the EIA, the anomaly effect is more pronounced at Tucumán than at São José dos Campos. The differences encountered between these very close stations suggest that in this sector relevant longitudinal-dependent variations could occur, with the longitudinal gradient of the Equatorial Electrojet that plays a key role to explain such differences together with the 5.8° separation in dip latitude between the two ionosondes. Furthermore at Tucumán, the daily peak value of NmF2 around 21:00 LT during equinox for HSA is in temporal coincidence with an impulsive enhancement of hmF2, showing a kind of “elastic rebound” under the action of the EIA. IRI-2012 and NeQuick2 bottom side profiles show significant deviations from ionosonde observations. In particular, both models provide a clear underestimation of the EIA strength at both stations, with more pronounced differences for Tucumán. Large discrepancies are obtained for the parameter hmF2 for HSA during daytime at São José dos Campos, where clear underestimations made by both models are observed. The shape parameter B₀ is quite well described by the IRI-2012 model, with very good agreement in particular during equinox for both stations for both LSA and HSA. On the contrary, the two models show poor agreements with ionosonde data concerning the shape parameter B₁.     

Longitudinal behaviors of the IRI-B parameters of the equatorial electron density profiles retrieved from FORMOSAT-3/COSMIC radio occultation measurements

The electron density profiles in the bottomside F₂-layer ionosphere are described by the thickness parameter B0 and the shape parameter B1 in the International Reference Ionosphere (IRI) model. We collected the ionospheric electron density (N_e) profiles from the FORMOSAT-3/COSMIC (F3/C) radio occultation measurements from DoY (day number of year) 194, 2006 to DoY 293, 2008 to investigate the daytime behaviors of IRI-B parameters (B0 and B1) in the equatorial regions. Our fittings confirm that the IRI bottomside profile function can well describe the averaged profiles in the bottomside ionosphere. Analysis of the equatorial electron density profile datasets provides unprecedented detail of the behaviors of B0 and B1 parameters in equatorial regions at low solar activity. The longitudinal averaged B1 has values comparable with IRI-2007 while it shows little seasonal variation. In contrast, the observed B0 presents semiannual variation with maxima in solstice months and minima in equinox months, which is not reproduced by IRI-2007. Moreover, there are complicated longitudinal variations of B0 with patterns varying with seasons. Peaks are distinct in the wave-like longitudinal structure of B0 in equinox months. An outstanding feature is that a stable peak appears around 100°E in four seasons. The significant longitudinal variation of B0 provides challenges for further improving the presentations of the bottomside ionosphere in IRI.     

Stimulation of plasma waves in the magnetosphere using satellite JIKIKEN (EXOS-B)

The stimulated plasma wave experiment (SPW) has been successfully carried out in the plasmasphere and the magnetosphere along the JIKIKEN (EXOS-B) satellite orbit where the plasma parameters indicate wide variety of the combination of the electron number density, ranging from 1/cc to 10⁴/cc, and the electron cyclotron frequency, ranging from 6 kHz to 200 kHz.The upper hybrid resonances F_UHR usually persists for long periods up to 125 msec and the electron cyclotron resonances nF_H are stimulated at frequencies with the very high harmonic number n; sometimes, the nF_H resonance takes place for n=47.All the features of the resonances including F_On reflect the characteristics of the magnetospheric plasma that contains the energetic and non-Maxwellian components of the particles. The measurement of the plasma resonance contributes to the detection of the local electron density and the magnetic field intensity. The mode of the propagating radio waves is also determined being compared with the observed local plasma resonance frequency F_p.