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。     

2219铝合金静止轴肩搅拌摩擦焊接头组织及性能

文摘采用静止轴肩搅拌摩擦焊的方法获得了2219C10S铝合金焊接接头,研究了焊接接头典型的宏观、微观组织特征、焊接工艺参数对焊缝成形特征及焊接接头力学性能的影响规律。结果表明:相对常规搅拌摩擦焊,由于静止轴肩式搅拌头的结构特点,焊接过程中可有效避免飞边和焊缝内部缺陷;随着焊速的增加,接头焊核由"碗状"变为"腰鼓"状,体积也逐渐减小,还出现了轴肩影响区这一特殊组织特征;焊接接头的显微硬度分布呈现出独特的"∪"形,焊核区的显微硬度最低;当焊接速度≤250 mm/min,随着焊接速度的增加,接头的拉伸性能逐渐增加;当焊接速度增加至300 mm/min时,由于在焊接接头中出现了沟槽缺陷,拉伸性能急剧下降。     

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。     

铝锂合金搅拌摩擦焊搭接接头组织及力学性能

采用搅拌摩擦焊对2mm厚不同铝锂合金进行搭接,并对接头的组织和力学性能进行分析。同时研究了焊接工艺参数、热处理状态对接头性能的影响。研究表明:搭接接头焊核区呈"洋葱环"结构,由细小的等轴晶组织构成;前进侧搭接界面有"钩状"缺陷,对接头力学性能产生不良影响。搭接接头的塑性较差,伸长率仅有3.18%,不及母材伸长率的25%;当转速为800r/min、焊速为200mm/min时,接头的强塑性最佳,抗拉强度达到467MPa(母材的94%);热处理对搅拌摩擦焊焊接头力学性能影响显著,经过人工时效后,接头强度提高了13%～18%,抗拉强度最高达到526MPa,伸长率都有所下降。断口形貌分析表明:接头拉伸断裂是从前进侧的"钩状"缺陷起裂;接头拉伸断口为准解理和韧窝断裂的复合断口。     

AZ31镁合金搅拌摩擦焊接头焊核区域成型过程及影响因素

接头焊核区域的形成是搅拌摩擦焊接的一个典型特征,其形状和大小对搅拌摩擦焊接头的性能有重要影响。以AZ31镁合金为母材,分析不同焊接参数(包括焊接压力、焊接速度、搅拌头倾斜角)条件下搅拌摩擦焊接头焊核成型的规律及特点,并建立焊核成型过程的简单模型。分析认为焊接压力和搅拌头倾斜角是影响焊核成型的重要因素,而焊接压力决定塑性材料的形成。焊核的形状主要由塑性材料的流动状态决定,搅拌头的形状和焊接速度影响塑性材料的流动,从而影响焊核的成型。掌握FSW焊核成型规律,可以选择合理的工艺参数。     

双脉冲MIG焊对2195Al-Li合金焊缝组织及性能的影响

研究了双脉冲MIG焊工艺对2195高强铝锂合金焊缝组织及性能的影响,通过焊后热处理工艺大幅提高了接头的力学性能。实验结果表明,在合适的双脉冲MIG焊工艺参数下,焊缝金属得到了大量的细小等轴晶组织,柱状晶数量明显减少,接头力学性能得到了提高。510℃×1h固溶＋150℃×11h时效焊后热处理后,接头性能得到进一步提升。     

TC4钛合金扩散焊接头的力学性能

在温度为910℃,压力为3.4MPa条件下对TC4钛合金板材进行了扩散焊接,对获得的扩散焊接头取样进行金相观察,仅在接近接头表面材料深度为1mm范围内发现未焊合缺陷,其余部分焊合较好,表明在给定工艺下可获得质量良好的焊接头.随后对TC4扩散焊接头的力学性能进行了试验研究,分别开展了静拉伸试验、断裂韧性试验及焊缝附近区域的纳米压痕试验.试验结果表明,所制得的TC4扩散焊接头屈服强度为887MPa,抗拉强度为948MPa,断裂韧性为101.9MPa·m1/2,均与原材料的性能相差不大.纳米压痕试验的结果显示,接头焊缝区和母材区的显微弹性模量分别为180.2GPa和178.0GPa.      

钛合金带筋壁板穿透焊工艺研究

从焊前准备、焊接装配、焊接保护、焊后校形、力学性能等5个方面,研究了钛合金穿透焊工艺及其焊接工艺参数,分析了焊接接头的组织性能。结果表明,充分的焊前准备、正确的焊接装配、有效的焊接保护及合理的焊接工艺参数是获得优质钛合金焊接接头的保证;焊后正确的热处理是零件保形的必要条件。     

铝合金可回抽搅拌摩擦焊接头组织和性能

针对8 mm 厚2219 铝合金进行可回抽搅拌摩擦焊工艺试验,详细分析了回抽过程中搅拌针运动

轨迹、不同回抽位置的接头组织形态及力学性能。结果表明:搅拌针的运动轨迹是焊接速度与搅拌针相对于轴

肩回抽速度的合成运动轨迹,并呈现出一定的线性关系。回抽结束处和回抽起始处的接头组织形貌为典型的

常规搅拌摩擦焊接头,位于中间回抽区域的焊接接头可以认为是100% 焊透的焊接接头与“相同直径的轴肩+

(100% ~0%) ×L 的搅拌针”形成的焊透深度逐渐变浅的常规搅拌摩擦焊接头复合形成的。接头力学性能测

试结果表明:回抽结束处的性能最高,回抽起始处的性能次之,中间回抽区域的力学性能最低,并且随着回抽距

离的逐渐增加,中间回抽区域的力学性能逐渐增加。不同回抽位置的搅拌摩擦焊接头均呈现出典型的韧性断

裂形貌。

     

BT20钛合金激光焊技术研究

针对2.5 mm厚BT20钛合金进行了CO2激光焊和YAG激光焊研究,结果表明由于激光特性不同,形成的焊缝几何特征不同,当焊接工艺适当,可保证焊接过程的稳定性和焊接接头的质量.在激光自熔焊时主要的焊缝缺陷是咬边,这是由于钛合金物理性能和激光高能束流焊特性所致.这种咬边缺陷不利于焊接接头性能,尤其是接头的疲劳性能和断裂韧性.采用活性剂和填丝焊,以及激光旋扫焊可以改善焊缝咬边缺陷,提高钛合金激光焊接头的力学性能.     

桨叶实度及轴间距对摆线桨气动特性影响研究

悬停状态下,设计参数和摆线桨间距离对摆线桨的气动特性有较大影响。首先通过算例验证滑移网格计算方法应用于摆线桨悬停状态下气动力计算的准确性,然后研究摆线桨在不同半径、弦长和桨叶数时的气动参数特性,最后计算分析不同距离时,摆线桨间的气动干扰特性。结果表明:随着半径增大,桨叶气动力和单位面积上载荷均增大;弦长越大,气动力越大,桨叶单位面积上载荷反而越小;4叶片摆线桨产生的气动力比3叶片和6叶片大,而3叶片的桨叶载荷最大;合力偏转角分别随转速和实度的增大而减小;随着摆线桨间距离的增加,气动力损失系数和合力偏转角均减小。     

Effects of Alloying Elements Ti, Cr, Al, and Hf on β-Nb5Si3 from First-principles Calculations

The energy, lattice parameters, electronic structures, and elastic constants of the intermetallic compound β-Nb₅Si₃ alloyed by Ti, Cr, Al, and Hf elements are investigated using first-principles methods based on plane-wave pseudopotential theory. From the impurity formation energy calculated, it is found that Ti, Cr, and Hf prefer to occupy the Nb_I, Nb_I, and Nb_II site, respectively, and that Al decreases the stability of β-Nb₅Si₃. Ti and Cr atoms reduce the c/a ratio of crystal lattices and Hf atom transforms the crystal lattice of β-Nb₅Si₃ from the tetragonal system to the orthorhombic system. The total state density of pure β-Nb₅Si₃ system and Ti, Cr, and Hf doped systems shows that Ti, Cr, and Hf improve the conductibility of β-Nb₅Si₃ system. The bulk modulus, shear modulus, and elastic modulus are obtained using Voight approximation equation. Ti and Cr increase the hardness and reduce the ductility of β-Nb₅Si₃. In contrast, Hf decreases the hardness and improves the ductility.     

Instability characteristics of a co-rotating wingtip vortex pair based on bi-global linear stability analysis

The Stereo Particle Image Velocimetry (SPIV) technology is applied to measure the wingtip vortices generated by the up-down symmetrical split winglet. Then, the temporal bi-global Linear Stability Analysis (bi-global LSA) is performed on this nearly equal-strength co-rotating vortex pair, which is composed of an upper vortex (vortex-u) and a down vortex (vortex-d). The results show that the instability eigenvalue spectrum illustrated by (ω_r, ω_i) contains two types of branches: discrete branch and continuous branch. The discrete branch contains the primary branches of vortex-u and vortex-d, the secondary branch of vortex-d and coupled branch, of which all of the eigenvalues are located in the unstable half-plane of ω_i > 0, indicating that the wingtip vortex pair is temporally unstable. By contrast, the eigenvalues of the continuous branch are concentrated on the half-plane of ω_i < 0 and the perturbation modes correspond to the freestream perturbation. In the primary branches of vortex-u and vortex-d, Mode P_u and Mode P_d are the primary perturbation modes, which exhibit the structures enclosed with azimuthal wavenumber m and radial wavenumber n, respectively. Besides, the results of stability curves for vortex-u and vortex-d demonstrate that the instability growth rates of vortex-u are larger than those of vortex-d, and the perturbation energy of Mode P_u is also larger than that of Mode P_d. Moreover, the perturbation energy of Mode P_u is up to 0.02650 and accounts for 33.56% percent in the corresponding branch, thereby indicating that the instability development of wingtip vortex is dominated by Mode P_u. By further investigating the topological structures of Mode P_u and Mode P_d with streamwise wavenumbers, the most unstable perturbation mode with a large azimuthal wavenumber of m = 5–6 is identified, which imposes on the entire core region of vortex-u. This large azimuthal wavenumber perturbation mode can suggest the potential physical-based flow control strategy by manipulating it.     

Microstructure and Mechanical Properties of In-situ Synthesized Al2O3/TiAl Composites

Al2O3 particle-reinforced TiAl composites are successfully reaction-synthesized from the powder mixture of Ti, Al, TiO2, and Nb2O5, using the hot pressing reaction synthesis technique. The microstructure and mechanical properties of the as-sintered products are investigated. It is found that in the as-sintered products consisting of γ-TiAl, α2-Ti3Al, Al2O3, and NbAl3 phases, the fine Al2O3 particles tend to disperse on the grain boundaries. With the Nb2O5 content increasing, the grains are remarkably refined and the Al2O3 particles are dispersing more uniformly in the TiAl matrix, forming a partial lamellar structure containing α and lamellar phases. The hardness of the in-situ composites increases gradually, and the bending strength and the fracture toughness of the as-sintered products reach the maximum value of 398.5 MPa and 6.99 MPa·m^1/2, respectively, as the Nb2O5 content increases to 6 wt%.     

Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R _S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm² sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5^∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm² sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm² sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm² sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R _S every 2–3 h (every ∼10 min from ∼20 R _S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date.     

多级考虑冷气掺混流片变厚度的S_1流面研究

为减少气冷涡轮气动设计难度,提出一套基于多级气冷涡轮考虑冷气掺混及随流道翘曲、变厚度的S1流面计算思路,编制了带冷气的翘曲S1流面薄片计算的参数化方法程序及网格自动生成程序,改良了传统平面薄片,对比分析了改良后平面薄片、翘曲S1流面薄片以及三维计算间差异,对某高压涡轮进行了翘曲S1流面薄片气动优化.结果显示:与三维计算对比,改良后平面薄片最大流量差距为22.68%,翘曲S1流面薄片为3.58%,一维数据上翘曲S1流面薄片更逼近三维计算;型面压力分布及马赫数云图分布上翘曲面S1流面薄片较改良后平面薄片更贴近三维计算;采用翘曲S1流面薄片进行优化后,效率较原始方案提升0.41%,流量较原始方案仅增加0.21%.     

The Cool Interstellar Medium

Infrared spectroscopy and photometry with ISO covering most of the emission range of the interstellar medium has led to important progress in the understanding of the physics and chemistry of the gas, the nature and evolution of the dust grains and also the coupling between the gas and the grains. We review here the ISO results on the cool and low-excitation regions of the interstellar medium, where T _gas≲ 500 K, n _H∼ 100–10⁵ cm⁻³ and the electron density is a few 10⁻⁴. JEL codes: D24, L60, 047 Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands, and the United Kingdom), and with the participation of ISAS and NASA.     

Microstructure evolution of a hypereutectic Nb–Ti–Si–Cr–Al–Hf alloy processed by directional solidification

In this work, the Nb–14Si–24Ti–10Cr–2Al–2Hf–0.1Y alloy(at.%) was processed by the liquid–metal-cooled directional solidification(DS) at 1750 C with withdrawal rates of 1.2, 6,18 mm/min and post heat treatment(HT) at 1450 C for 10 h. The microstructures of the directionally solidified and heat treated samples were investigated. The results show that the microstructure of directionally solidified alloy mainly consists of petaloid Nbss+ Nb5Si3eutectics and Ti-rich Nbss+ Nb5Si3+ Cr2Nb eutectics. With the increase of withdrawal rate, the primary Nb5Si3is eliminated, Nbss+ Nb5Si3eutectic cells turn round and connected with the microstructure refinement and Nbss+ Nb5Si3+ Cr2Nb eutectics turn to a river-like morphology. After heat treatment,Nbss+ Nb5Si3+ Cr2Nb eutectics disappeared and petaloid Nbss+ Nb5Si3eutectics turn to a specific fiber-mesh structure gradually, which is promoted by higher withdrawal rates. Furthermore,both the volume fraction of Cr2Nb and the content of Cr in Nbssof Nbss+ Nb5Si3eutectics change regularly with the increase of withdrawal rate and heat treatment at 1450 C for 10 h.     

Deep Impact: Working Properties for the Target Nucleus – Comet 9P/Tempel 1

In 1998, Comet 9P/Tempel 1 was chosen as the target of the Deep Impact mission (A’Hearn, M. F., Belton, M. J. S., and Delamere, A., Space Sci. Rev., 2005) even though very little was known about its physical properties. Efforts were immediately begun to improve this situation by the Deep Impact Science Team leading to the founding of a worldwide observing campaign (Meech et al., Space Sci. Rev., 2005a). This campaign has already produced a great deal of information on the global properties of the comet’s nucleus (summarized in Table I) that is vital to the planning and the assessment of the chances of success at the impact and encounter. Since the mission was begun the successful encounters of the Deep Space 1 spacecraft at Comet 19P/Borrelly and the Stardust spacecraft at Comet 81P/Wild 2 have occurred yielding new information on the state of the nuclei of these two comets. This information, together with earlier results on the nucleus of comet 1P/Halley from the European Space Agency’s Giotto, the Soviet Vega mission, and various ground-based observational and theoretical studies, is used as a basis for conjectures on the morphological, geological, mechanical, and compositional properties of the surface and subsurface that Deep Impact may find at 9P/Tempel 1. We adopt the following working values (circa December 2004) for the nucleus parameters of prime importance to Deep Impact as follows: mean effective radius = 3.25± 0.2 km, shape – irregular triaxial ellipsoid with a/b = 3.2± 0.4 and overall dimensions of ∼14.4 × 4.4 × 4.4 km, principal axis rotation with period = 41.85± 0.1 hr, pole directions (RA, Dec, J2000) = 46± 10, 73± 10 deg (Pole 1) or 287± 14, 16.5± 10 deg (Pole 2) (the two poles are photometrically, but not geometrically, equivalent), Kron-Cousins (V-R) color = 0.56± 0.02, V-band geometric albedo = 0.04± 0.01, R-band geometric albedo = 0.05± 0.01, R-band H(1,1,0) = 14.441± 0.067, and mass ∼7×10¹³ kg assuming a bulk density of 500 kg m⁻³. As these are working values, {i.e.}, based on preliminary analyses, it is expected that adjustments to their values may be made before encounter as improved estimates become available through further analysis of the large database being made available by the Deep Impact observing campaign. Given the parameters listed above the impact will occur in an environment where the local gravity is estimated at 0.027–0.04 cm s⁻² and the escape velocity between 1.4 and 2 m s⁻¹. For both of the rotation poles found here, the Deep Impact spacecraft on approach to encounter will find the rotation axis close to the plane of the sky (aspect angles 82.2 and 69.7 deg. for pole 1 and 2, respectively). However, until the rotation period estimate is substantially improved, it will remain uncertain whether the impactor will collide with the broadside or the ends of the nucleus.