基于超声波C 扫描的SUS304 不锈钢板点焊接头质量分析

利用超声波水浸聚焦入射法对1 mm厚的SUS304奥氏体不锈钢板点焊接头进行超声C扫描成像检测;研究了不同焊接工艺参数下获得点焊接头的超声波C扫描图像特征,据此分析了接头的焊核直径,并与焊核切口端面尺寸进行了比较;对点焊接头进行了拉伸—剪切试验,测试了接头的力学性能。结果表明:超声波水浸聚焦入射法能够观测出点焊焊核直径,并能有效地观测出焊核内部形貌特征。当焊接电流为定值(4k A),供给压力为0.15 MPa时,接头出现飞溅、焊穿等缺陷,并且在超声波C扫描图像中能够清晰地反映出来;当供给压力为0.45 MPa时,虽然点焊焊核直径增大,且未出现焊接缺陷,但是过大的供给压力导致接头厚度变小,影响了接头抗拉强度。当供给压力为定值(0.4 MPa),焊接电流为9 k A时,在C扫描图像上同样反映出飞溅、焊穿等典型的焊接缺陷,此时接头的失效载荷及能量吸收值急剧下降。     

基于 SAM 的不锈钢点焊接头无损检测

运用超声波扫描显微镜(SAM)对1 mm厚SUS304不锈钢薄板点焊接头进行无损检测,分析不同焊接工艺条件下的C扫描图像,并对C扫描图像各特征区域的A扫描信号进行采集、分析,研究两者间的对应关系,通过超声波C扫描成像法对焊核直径进行测量。结果表明:超声波扫描显微镜可以检测不锈钢点焊接头缺陷,并通过C扫描图像区分缺陷类型;在电极压力为0.15 MPa、焊接电流大于8 k A时,C扫描图像可以清楚的反映飞溅、过烧等缺陷;C扫描图像各特征区域表现出不同的A扫描信号特征;基于超声波C扫描测量的焊核直径为4.39~5.25 mm。     

钎焊温度对C/C/AgCuTi+Cf/TC4接头组织及力学性能的影响

为了缓解C/C复合材料与TC4合金钎焊接头的残余应力,采用AgCuTi+0.3％Cf钎料实现了二者的连接.使用扫描电子显微镜、透射电子显微镜确定了界面微观组织结构,利用万能试验机表征接头的力学性能,对不同钎焊温度下的接头界面组织及力学性能进行了分析,并归纳了钎焊接头形成过程,阐明了碳纤维在接头形成过程中的作用机理.结果...     

点焊接头超声C扫描图像分析及焊核直径测量

采用超声波扫描显微镜获取了点焊接头C扫描图像,分析点焊接头C扫描图像灰度值的分布特征,提出了一种对焊核边缘、焊核直径进行快速检测分析的方法;对不同焊接工艺参数下的不锈钢点焊接头进行表面检测,对比分析基于C扫描图像的焊点检测结果与实际测量值。结果表明,通过这种测量方法不但可以快速得到焊核边缘及焊核尺寸,而且避免了人为因素的影响;与实际测量结果相对比,两者之间相差较小,证实了该检测方法的可行性。     

界面端奇异应力场分析在异种材料焊接中的应用

依据界面力学的奇异性理论,阐述了接触角为90°的对接界面的奇异应力场特征,并以此为基础,分别对异种钛合金的线性摩擦焊材料选用、Cf/C复合材料与TC4钛合金钎焊接头的钎料选择及界面层设计进行了分析,结果表明:TC4/TC17较TC11/TC17具有较好的界面匹配,更易获得良好的线性摩擦焊接头;选用AgCuTi钎料较TiZrNiCu钎料更适于Cf/C复合材料与TC4合金的钎焊;选用TiZrNiCu钎料时,采用Cf/C复合材料/TiZrNiCu/Cu/TiZrNiCu/Mo/TiZrNiCu/TC4界面结构进行钎焊可获得较好的匹配连接。     

超声干涉法薄层厚度测量声阻抗匹配判据及其应用

针对超声干涉法测量薄层厚度的原理,讨论了薄层及与其相邻介质声阻抗匹配分别满足界面声压反射系数|R1|＜1/2或|R1|＞1/2时回波信号的选取原则,并以薄层声压反射系数谱为依据,分析了上述两种声阻抗匹配条件下谱线分别出现次生极大或极小值的规律,在此基础上提出了薄层厚度测量时谱线极值的选择方法.以航空雷达罩蒙皮GFRP(Glass Fiber Reinforced Plastic)层板外表面复合涂层以及钢基体表面ZrO2陶瓷涂层样品为例进行了薄层厚度测量实验研究及信号分析.研究表明,超声干涉法薄层厚度实验结果与SEM(Scanning Electron Microscope)测量结果相符.由此可知,薄层及与其相邻介质声阻抗匹配判据对于超声干涉法薄层厚度测量具有很强的理论指导意义及工程应用价值.     

激光毛化对Cf/SiC与TC4钎焊接头组织及性能的影响

由于线胀系数差异大,Cf/Si C复合材料与TC4钛合金钎焊接头容易形成较大的内应力而开裂失效。为了进一步提高接头强度,应用激光毛化工艺在Cf/Si C表面烧蚀出微孔,采用银基钎料对Cf/Si C与TC4进行钎焊。焊后对接头力学性能进行测试,对接头界面及断口显微组织进行观察。结果表明:焊前对Cf/Si C表面进行激光毛化处理,钎料能够填充微孔并形成良好的钎焊界面,能够提高Cf/Si C与TC4钎焊接头的剪切强度。     

表面改性C/C复合材料与LAS玻璃陶瓷的连接

采用MgOAl₂O₃SiO₂(MAS)玻璃作为中间层,对SiCMoSi₂表面改性的C/C复合材料与Li₂CO₃Al₂O₃SiO₂(LAS)玻璃陶瓷进行热压连接。通过正交实验,研究了连接温度、连接压力和保温时间对试样连接强度的影响,确定最佳工艺参数为：1 200 ℃,20 MPa,15 min,所得到连接接头的最高剪切强度可达30 MPa。利用扫描电子显微镜（SEM）、能谱仪（EDS）和背散射电子像（BEI)对SiCMoSi₂涂层、连接界面的形貌以及组成进行了分析。研究结果表明,SiCMoSi₂涂层与基体结合紧密,Si,C元素在界面处呈梯度状分布,形成厚度约为15 μm的过渡层。MAS玻璃中的组分与LAS玻璃陶瓷和SiCMoSi₂涂层存在相互渗透现象,形成紧密的C/C(SiCMoSi₂)/MAS/LAS结构,界面间的结合良好。     

涡流C扫描在钛合金SPF/DB结构检测中的实验研究

为了探索SPF/DB结构检测中有效的检测方法,应用涡流C扫描对钛合金SPF/DB结构进行了检测实验,将涡流C扫描结果和SPF/DB结构检测中常用的超声C扫描结果进行了对比分析。结果表明,涡流C扫描能够检测出SPF/DB结构的界面宏观缺欠以及一定尺度以上的界面微观缺欠,在SPF/DB结构检测中是可行的。有必要对该检测方法的有效性和检测结果的可靠性进行深入研究。     

多向编织C/ C 复合材料显微结构的滋-CT 研究

以多向编织C/C复合材料为研究对象,对其内部组织结构进行了CT扫描,通过对投影旋转中心校正、噪声抑制、环状伪影校正等数据进行了处理.结果表明:经过处理数据,图像质量明显改善,提高了材料内部微结构细节的辨识程度,为C/C复合材料内部微结构三维重构提供了良好的基础.     

Fatigue crack propagation of new aluminum lithium alloy bonded with titanium alloy strap

A new type of aluminum lithium alloy (Al-Li alloy) Al-Li-S-4 was investigated by test in this paper. Alloy plate of 400 mm · 140 mm · 6 mm with single edge notch was made into samples bonded with Ti-6Al-4V alloy (Ti alloy) strap by FM 94 film adhesive after the surface was treated. Fatigue crack growth of samples was investigated under cyclic loading with stress ratio (R) of 0.1 and load amplitude constant. The results show that Al-Li alloy plate bonded with Ti alloy strap could retard fatigue crack propagation. Retardation effect is related with width and thickness of strap. Flaws have an observable effect on crack propagation direction.     

军用航空有机玻璃热分析动力学研究

对某型号军用飞机上航空有机玻璃用热重-差热(TG-DTA)分析仪进行了热分析动力学研究,实验在不同的氧气浓度(5%,10%,15%,21%)和升温速率(15℃/min,30℃/min)条件下进行,用改良的Coats-Redfern法计算出了动力学参数,用Doyle法计算理论失重值。研究发现表观活化能和频率因子都随氧浓度的下降而增加,在升温度速率分别为15℃/min和30℃/min条件下当氧浓度变化时表观活化能分别为100~108kJ/mol和87~92kJ/mol,而频率因子分别为(7~35)10⁶/s和(0.4~1)10⁶/s。计算结果很好的吻合了实验结果。     

定向破坏复合材料层合壳体结构铺层的分析与设计

以复合材料层合板为基本材料设计了一种结构新颖的定向破坏复合材料层合壳体结构,在导弹与

该壳体结构的初始接触区域预制缺陷区,导弹发射时以四瓣形式开裂,大幅度提高了导弹的发射效率。利用ANSYS

有限元模拟分析软件,通过强度分析确定了最佳铺层设计方案,单层板厚度为0.2 mm,采用基体本身加强预

置缺陷区的[0°/90°/ ±45°]2S 铺层方式。该种铺层方式的爆破载荷为0.21 MPa,最小顶破载荷为1 kN,完全能够

满足其在工作环境下既能承受一定的压力不漏气又能在较小的顶破载荷下自行破裂的设计要求。

     

Auroral Substorms: Search for Processes Causing the Expansion Phase in Terms of the Electric Current Approach

Auroral substorms are mostly manifestations of dissipative processes of electromagnetic energy. Thus, we consider a sequence of processes consisting of the power supply (dynamo), transmission (currents/circuits) and dissipations (auroral substorms-the end product), namely the electric current line approach. This work confirms quantitatively that after accumulating magnetic energy during the growth phase, the magnetosphere unloads the stored magnetic energy impulsively in order to stabilize itself. This work is based on our result that substorms are caused by two current systems, the directly driven (DD) current system and the unloading system (UL). The most crucial finding in this work is the identification of the UL (unloading) current system which is responsible for the expansion phase. A very tentative sequence of the processes leading to the expansion phase (the generation of the UL current system) is suggested for future discussions.

1. (1)
   The solar wind-magnetosphere dynamo enhances significantly the plasma sheet current when its power is increased above \(10^{18}~\mbox{erg}/\mbox{s}\) (\(10^{11}\) w).
    
2. (2)
   The magnetosphere accumulates magnetic energy during the growth phase, because the ionosphere cannot dissipate the increasing power because of a low conductivity. As a result, the magnetosphere is inflated, accumulating magnetic energy.
    
3. (3)
   When the power reaches \(3\mbox{--}5\times 10^{18}~\mbox{erg}/\mbox{s}\) (\(3\mbox{--}5\times 10^{11}\) w) for about one hour and the stored magnetic energy reaches \(3\mbox{--}5\times10^{22}\) ergs (\(10^{15}\) J), the magnetosphere begins to develop perturbations caused by current instabilities (the current density \({\approx}3\times 10^{-12}~\mbox{A}/\mbox{cm}^{2}\) and the total current \({\approx}10^{6}~\mbox{A}\) at 6 Re). As a result, the plasma sheet current is reduced.
    
4. (4)
   The magnetosphere is thus deflated. The current reduction causes \(\partial B/\partial t > 0\) in the main body of the magnetosphere, producing an earthward electric field. As it is transmitted to the ionosphere, it becomes equatorward-directed electric field which drives both Pedersen and Hall currents and thus generates the UL current system.
    
5. (5)
   A significant part of the magnetic energy is accumulated in the main body of the magnetosphere (the inner plasma sheet) between 4 Re and 10 Re, because the power (Poynting flux \([ \boldsymbol{E} \times \boldsymbol{B} ])\) is mainly directed toward this region which can hold the substorm energy.
    
6. (6)
   The substorm intensity depends on the location of the energy accumulation (between 4 Re and 10 Re), the closer the location to the earth, the more intense substorms becomes, because the capacity of holding the energy is higher at closer distances. The convective flow toward the earth brings both the ring current and the plasma sheet current closer when the dynamo power becomes higher.
    

This proposed sequence is not necessarily new. Individual processes involved have been considered by many, but the electric current approach can bring them together systematically and provide some new quantitative insights.

     

摆盘流动与换热性能数值仿真

针对受燃烧室出口高温燃气冲刷的摆盘装置的冷却水回路,建立二维、三维物理仿真模型,模拟了冷却水在内部流道的 流动与换热过程,考察了冷却水进口压力、冷却水流量对流阻和换热性能的影响.结果表明:①摆盘冷却水进口压力由2.3×105Pa提高到8.3×105Pa,摆盘壁温变化微小,结构1壁温升高5K,结构2壁温升高7K;②冷却水进口速度由0.5m/s提高到5.3m/s,结构1壁温降低约120K,结构2壁温降低约100K,冷却效果明显;③结构2通过缩小流道的流通面积,能在更小的冷却水流量的工况下得到更好的换热效果.      

Ion Temperatures as Observed in a Solar Coronal Hole

From the widths of the extreme ultraviolet (EUV) lines measured by the SUMER instrument on SOHO, it was found previously (Tu et al. 1998) that the average temperature of Ne⁺⁷, at heights (relative to h₀) above the southern solar limb from 17″ to 64″, ranges between 1.3 and 5 × 10⁶ K and of Ne⁺⁶ between 1 and 4 × 10⁶ K. For mass-per-charge numbers greater than 4 the temperatures of the ions increase slightly with increasing mass-per-charge, while the thermal speed reveals no clear trend. We present a new data set with exposure times much longer than the ones in the previous study. The results obtained from line width analysis of Fe XII (1242 Å), Mg X (1249 Å), Mg VIII (772 Å) Ne VIII (770 Å), and Si VIII (1445 Å) support our previous study. In this case, the trend of increasing temperature begins at a mass-per-charge number of 3. A qualitative explanation based on ion-cyclotron-resonance heating within linear kinetic theory is suggested.     

Measuring Black Hole Spin Using X-Ray Reflection Spectroscopy

I review the current status of X-ray reflection (a.k.a. broad iron line) based black hole spin measurements. This is a powerful technique that allows us to measure robust black hole spins across the mass range, from the stellar-mass black holes in X-ray binaries to the supermassive black holes in active galactic nuclei. After describing the basic assumptions of this approach, I lay out the detailed methodology focusing on “best practices” that have been found necessary to obtain robust results. Reflecting my own biases, this review is slanted towards a discussion of supermassive black hole (SMBH) spin in active galactic nuclei (AGN). Pulling together all of the available XMM-Newton and Suzaku results from the literature that satisfy objective quality control criteria, it is clear that a large fraction of SMBHs are rapidly-spinning, although there are tentative hints of a more slowly spinning population at high (M>5×10⁷ M _⊙) and low (M<2×10⁶ M _⊙) mass. I also engage in a brief review of the spins of stellar-mass black holes in X-ray binaries. In general, reflection-based and continuum-fitting based spin measures are in agreement, although there remain two objects (GRO J1655–40 and 4U 1543–475) for which that is not true. I end this review by discussing the exciting frontier of relativistic reverberation, particularly the discovery of broad iron line reverberation in XMM-Newton data for the Seyfert galaxies NGC 4151, NGC 7314 and MCG–5-23-16. As well as confirming the basic paradigm of relativistic disk reflection, this detection of reverberation demonstrates that future large-area X-ray observatories such as LOFT will make tremendous progress in studies of strong gravity using relativistic reverberation in AGN.     

The Burst Alert Telescope (BAT) on the SWIFT Midex Mission

he burst alert telescope (BAT) is one of three instruments on the Swift MIDEX spacecraft to study gamma-ray bursts (GRBs). The BAT first detects the GRB and localizes the burst direction to an accuracy of 1–4 arcmin within 20 s after the start of the event. The GRB trigger initiates an autonomous spacecraft slew to point the two narrow field-of-view (FOV) instruments at the burst location within 20–70 s so to make follow-up X-ray and optical observations. The BAT is a wide-FOV, coded-aperture instrument with a CdZnTe detector plane. The detector plane is composed of 32,768 pieces of CdZnTe (4×4×2 mm), and the coded-aperture mask is composed of ∼52,000 pieces of lead (5×5×1 mm) with a 1-m separation between mask and detector plane. The BAT operates over the 15–150 keV energy range with ∼7 keV resolution, a sensitivity of ∼10⁻⁸ erg s⁻¹ cm⁻², and a 1.4 sr (half-coded) FOV. We expect to detect > 100 GRBs/year for a 2-year mission. The BAT also performs an all-sky hard X-ray survey with a sensitivity of ∼2 m Crab (systematic limit) and it serves as a hard X-ray transient monitor.     

The Grain Impact Analyser and Dust Accumulator (GIADA) Experiment for the Rosetta Mission: Design, Performances and First Results

The Grain Impact Analyser and Dust Accumulator (GIADA) onboard the ROSETTA mission to comet 67P/Churyumov–Gerasimenko is devoted to study the cometary dust environment. Thanks to the rendezvous configuration of the mission, GIADA will be plunged in the dust environment of the coma and will be able to explore dust flux evolution and grain dynamic properties with position and time. This will represent a unique opportunity to perform measurements on key parameters that no ground-based observation or fly-by mission is able to obtain and that no tail or coma model elaborated so far has been able to properly simulate. The coma and nucleus properties shall be, then, clarified with consequent improvement of models describing inner and outer coma evolution, but also of models about nucleus emission during different phases of its evolution. GIADA shall be capable to measure mass/size of single particles larger than about 15 μm together with momentum in the range 6.5 × 10⁻¹⁰ ÷ 4.0 × 10⁻⁴ kg m s⁻¹ for velocities up to about 300 m s⁻¹. For micron/submicron particles the cumulative mass shall be detected with sensitivity 10⁻¹⁰ g. These performances are suitable to provide a statistically relevant set of data about dust physical and dynamic properties in the dust environment expected for the target comet 67P/Churyumov–Gerasimenko. Pre-flight measurements and post-launch checkouts demonstrate that GIADA is behaving as expected according to the design specifications. The International GIADA Consortium (I, E, UK, F, D, USA).