起重船用高强钢大厚板焊接残余应力的试验研究

以某型起重船结构为研究对象,采用焊接后热作为焊接残余应力消除措施,研究结构的残余应力情况及消除措施的有效性。首先采用焊态和经过焊接后热的两组试板进行焊接残余应力检测并对比,结果表明焊态的试板焊接纵向残余应力最高达552.5 MPa,接近材料的屈服强度;经后热的试板纵向残余应力最大为385.3MPa,与焊态相比降低了167.2 MPa,下降约30%;同时获取了残余应力分布情况。进一步对起重船导向基座结构的焊缝进行后热并进行应力检测,其纵向焊接残余应力最大值为310.8 MPa,远低于母材屈服强度。本文研究表明：起重船高强钢大厚板在焊态时焊接残余应力较大,需采取措施消除残余应力;采用焊接后热可以大幅降低高强钢大厚板的焊接残余应力水平,焊接后热具有较好的经济性和操作便捷性,在起重船建造过程中建议考虑对大厚板焊缝进行后热以消除焊接残余应力消除。     

金属壳体支座角焊缝应力场数值模拟

文摘针对某固体发动机金属壳体支座焊接过程及热处理过程,利用通用ANSYS有限元分析软件对不同尺寸支座角焊缝应力场进行模拟计算。结果表明:支座焊后的应力主要集中在角焊缝热影响区处,应力水平较高,且随着支座尺寸的增加,残余应力显著增加;壳体经过退火和调质热处理后,角焊缝残余应力得到重新分布,整体残余应力较小。     

钛合金薄板激光修饰焊残余应力研究

采用X射线法测量焊接残余应力,对比研究了TC4钛合金薄板激光焊和激光修饰焊的残余应力分布规律与特点。结果表明:激光修饰焊未改变TC4钛合金薄板激光焊接接头残余应力的分布特征;激光修饰焊可以显著降低焊接接头横向残余应力,X方向上的最大残余压应力由原来的409MPa降到345MPa,Y方向则从316MPa降至278MPa,在焊缝两侧8mm范围内,应力值波动很小,基本呈现均匀分布,对于焊接纵向残余应力激光修饰焊只是略微降低应力波动幅度;与激光焊的接头边缘处相比,由于边缘效应激光修饰焊接产生的残余应力释放幅度较低,从27%~42%降到10%~18%。     

Ti_2AlNb合金电子束焊接接头的残余应力与再热裂纹

利用数值分析和试验测量方法研究了不同板厚和不同形状Ti_2AlNb合金电子束焊接接头的焊接应力,分析了再热裂纹的产生特点和焊后热处理过程中的组织演变,讨论了再热裂纹产生的原因。结果表明,电子束焊缝中心部位承受3向拉应力,纵向残余拉伸应力最大,超过1100MPa;横向拉伸应力较小;板较薄时厚度方向残余拉伸应力也较小,但当焊接厚板时焊缝中心厚度方向的残余拉伸应力也很大,深窄焊缝中可达1000MPa。同样板厚条件下,环形焊缝与直线焊缝相比,周向拉伸应力略小于纵向应力,但径向拉伸应力远大于横向应力,尤其是环的直径较小时。再热裂纹的产生与再热过程中晶界析出物及较高的拉伸应力有关,在加热速度低于一定值,加热到700℃左右时,裂纹沿晶界析出层与基体之间的界面产生与扩展。     

超声冲击载荷对CP3钛合金焊接接头残余应力的影响

首先建立了焊接过程及超声冲击过程有限元模型,得到超声冲击处理前后CP3钛合金焊接焊缝处残余应力分布规律;基于模拟仿真结果,进行了相应的工艺试验研究,以不同大小冲击载荷对焊缝处进行全覆盖冲击,采用小孔法测量不同处理条件下的残余应力值。结果表明,采用超声冲击处理方法,可将焊缝处的高值残余拉应力转化为压应力,残余应力降幅达到125%以上;随着冲击力的增加,压应力的幅值不断增大,但当冲击力达到60N后,压应力将趋于稳定,不再增加。     

钛合金电子束焊接表面残余应力的测试和有限元分析

采用多束电子束流焊接Ti60钛合金,并利用小孔法和有限元分析方法分别测试和模拟焊后残余应力值.对焊前预热、焊后缓冷和焊前预热+焊后缓冷三种焊接工艺下的残余应力值进行比较,研究残余应力的分布规律.研究结果表明,在垂直焊缝截面上,纵向残余应力σx的模拟结果与测试结果在变化趋势上基本一致.在平行焊缝截面上,实测与模拟纵向残余应力σx的分布规律相似.证明了有限元模型的合理性和可靠性.采用预热+焊接的焊接工艺对残余应力影响不大,采用焊接+缓冷的焊接工艺可以改变残余应力的分布.     

钛合金窄间隙TIG焊试板热处理前后表面残余应力研究

采用磁控窄间隙TIG焊接方法对31mm厚TC4钛合金试板进行焊接,焊接完成后采用压痕应变法测量真空退火处理前后表面焊接残余应力分布。结果表明,试板表面纵向焊接残余应力σx和横向焊接残余应力σy均较高;试板下表面焊接残余应力高于上表面焊接残余应力;峰值焊接残余应力出现在高温热影响区,数值可以达到材料屈服强度的50%~60%。经过650℃的真空退火热处理,焊接试板的纵向和横向残余应力均显著降低,残余应力降低幅度最高超过50%,剩余残余应力峰值均低于200MPa,表面残余应力重新分布。     

铝合金焊接结构的应力松弛及控制

针对生产现场大尺寸5A06-H112铝合金板箱形件拼焊制造过程中存在应力松弛的问题,对多种焊接工艺方法进行了研究.通过对不同焊接接头的力学性能试验、残余应力测试、焊接金相和硬度测量结果对比显示,铝合金焊接结构的应力变化存在先升后降的变化趋势,而TIG焊由于采用较小的线能量和多层焊,较MIG焊其应力松弛的程度存在差异.结果表明,增加焊后时效时间8～10d,并采用TIG焊技术将有效减小铝合金焊接结构的应力松弛,使端头下沉减少50％左右,满足了设计图纸的要求.     

贮箱壁板法兰盘装配及自动化焊接工艺

现有的壁板法兰盘焊接工装结构简单,压紧力小,并且为手工焊接,焊后法兰盘焊缝残余应力与变形大,质量稳定性差,不能满足型号使用需求。本文从影响法兰盘焊接质量因素入手,研制了法兰盘自动化焊接工装,在模拟仿真的基础上,得到0.15~0.25 mm的过盈装配量法兰盘与孔径采用的过盈量为最优,采用先装壁板后装法兰盘的流程可有效避免装配裂纹,并通过焊前加热垫板的方式解决法兰焊缝打底裂纹难题,采用自动焊工艺焊接的法兰成型美观,焊接缺陷比手工焊降低70%以上,接头低温平均抗拉强度达到348 MPa,延伸率为6.7%。     

铝合金动态控制低应力无变形（DC - LSND）MAG 焊焊接过程模拟

对动态控制低应力无变形（dynamically controlled low stress no - distortion,DC - LSND）铝合金 MAG 焊进行了数值仿真,利用数值仿真模型并结合优化算法对热沉参数进行了优化分析。通过对有限元软件的二次开发,实现了焊接热源程序的加载和热沉过程的加载。对比正常焊接过程,采用热沉实现了随焊激冷法后焊接残余应力降低。在其他条件热沉不变的条件下,随着热沉强度的增大,残余应力显著降低。在热沉强度不变的情况下,热沉与热源距离在30 mm 左右时,应力降低效果最为明显。     

捷变频磁控管用高频直线振荡电机设计

捷变频磁控管的快速捷变特性取决于驱动电机的性能,要求电机功耗小、体积小、效率高,能实现高频稳幅直线振动.文章介绍了音圈直线电机、电磁开关式直线电机和电磁混合式直线电机等三种方案,通过对其工作原理和性能特点分析,确定了音圈直线电机驱动方案,进行了电磁场仿真分析和电磁参数设计,进行了样机试验测试.结果表明,设计的音圈直线电...     

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。     

A new target tracking filter based on deep learning

At present, current filters can basically solve the filtering problem in target tracking, but there are still many problems such as too many filtering variants, too many filtering forms, loosely coupled with the target motion model, and so on. To solve the above problems, we carry out crossapplication research of artificial intelligence theory and methods in the field of tracking filters. We firstly analyze the computation graphs of typical a-β and Kalman. Through analysis, it is concluded that ...     

Investigations of entrainment characteristics and shear-layer vortices evolution in an axisymmetric rear variable area bypass injector

In this study,firstly,for the axisymmetric RVABI,the change-rule of adverse pressure gradient caused by radial velocity during the transition of internal flow mode in variable geometry is summarized,and a Bypass Ratio(BR) iterative algorithm based on the empirical correlation of non-equilibrium pressure is proposed.The algorithm can estimate the nonlinear relationship between area ratio and BR,with an error range falling below 6.5%.Then,we discuss the favorable effect of uniform mixing on the th...     

PVC糊树脂对交联PVC泡沫塑料的影响

通过水煮发泡制备交联聚氯乙烯泡沫塑料,讨论了聚氯乙烯(PVC)糊树脂对泡沫制备过程中经制糊、模压和发泡工艺得到的产物的影响,研究了PVC糊树脂对制备的交联PVC泡沫压缩性能的影响.结果表明:制备交联聚氯乙烯泡沫塑料适宜的糊黏度是4～9 Pa·s;PVC糊树脂的K值较大或水萃取液pH值呈碱性可有效防止模压过程中PVC的降解;PVC糊树脂的水萃取液pH值呈碱性可催化发泡反应,有利于得到低密度泡沫且缩短发泡时间;随着其K值增加,制备的泡沫压缩强度增大,但是K值过大时,制备的泡沫泡孔较大,压缩强度反而降低,适宜的K值为70～80.     

Alfvénic Electron Acceleration in Aurora Occurs in Global Alfvén Resonosphere Region

Auroral emission caused by electron precipitation (Hardy et al., 1987, J. Geophys. Res. 92, 12275–12294) is powered by magnetospheric driving processes. It is not yet fully understood how the energy transfer mechanisms are responsible for the electron precipitation. It has been proposed (Hasegawa, 1976, J. Geophys. Res. 81, 5083–5090) that Alfvén waves coming from the magnetosphere play some role in powering the aurora (Wygant et al., 2000, J. Geophys. Res. 105, 18675–18692, Keiling et al., 2003, Science 299, 383–386). Alfvén-wave-induced electron acceleration is shown to be confined in a rather narrow radial distance range of 4–5 R _E (Earth radii) and its importance, relative to other electron acceleration mechanisms, depends strongly on the magnetic disturbance level so that it represents 10% of all electron precipitation power during quiet conditions and increased to 40% during disturbed conditions. Our observations suggest that an electron Landau resonance mechanism operating in the “Alfvén resonosphere” is responsible for the energy transfer.     

Multiframe weak target track-before-detect based on pseudo-spectrum in mixed coordinates

Traditional multiframe Track-Before-Detect(TBD) may incur adverse integration loss resulting from model mismatch in sensor coordinates. Its suboptimal integration strategy may cause target envelope degradation. To address these issues, a pseudo-spectrum-based multiframe TBD in mixed coordinates is proposed firstly. The data search for energy integration is conducted based on an accurate model in the x-y plane while target energy is integrated based on pseudo-spectrum in sensor coordinates. The a...     

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.     

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.