一种热连轧GH4169合金的蠕变行为与断裂机制

通过蠕变性能测试及组织形貌观察,研究了热连轧直接时效处理的GH4169镍基合金的蠕变行为和断裂机制。结果表明:热连轧GH4169镍基合金的组织结构由γ′,γ″相和γ基体相组成,具有较小的晶粒尺寸,晶内存在高密度位错和孪晶。经直接时效后,合金中弥散分布的细小γ″相数量增加,及高密度位错引起的形变强化效果,是使合金在650℃/725MP条件下具有较长的蠕变寿命的主要原因;蠕变期间,合金的变形特征是孪晶变形和位错的双取向滑移;随着蠕变进行,位错的数量逐渐增加,并在晶界处引起应力集中,致使裂纹在晶界处萌生及扩展是合金的蠕变断裂机制。     

Ti-0.2Pd钛合金高温拉伸本构关系

采用高温拉伸试验,研究了Ti-0.2Pd在600～800°C,应变速率10-4～10-1s-1的高温流变行为。获得了流变应力与应变速率和变形温度的依存关系以及变形激活能Q为100.9kJ.mol-1,应力指数n为4.8。建立了Ti-0.2Pd合金热变形的理论基础。     

连续多试样纳米金刚石膜沉积设备及工艺

首先对热丝化学气相沉积(Chem ica l vapor depos ition,CVD)系统进行改造,设计了在真空室外对室内试样进行操纵的机械手系统和储料台,实现了一次热丝碳化后完成多个不同工艺条件下试样的连续沉积。有限元仿真研究结果表明,多衬底温度场比较均匀,适合于金刚石膜的生长。最后,采用改进沉积系统,在A r-CH4-H2气氛中,在多晶钼衬底上成功制备了纳米金刚石薄膜。R am an,XRD和AFM等结果表明,制备的金刚石纯度较高,晶粒大小在30 nm左右,表面光滑。     

轴流压气机非定常流及端壁边界层测量中的热线技术

本文总结了测量轴流压气机失速喘振工况及端壁边界层流场时所采用的方法,并提供若干典型结果。大量试验表明这些方法行之有效。用三支同型探针,沿周向不等间隔分布,失速喘振时,用频谱分析确定频率成分,用互相关分析确定两两信号的时差,即可判明是失速或喘振,并决定团数、团的传播速度及团的形状。用单丝旋转法测量端壁边界层以保证所测参数严格属于同一半径,同时又具有 X 型探针的二维能力,以测定速度矢量,湍流度及雷诺应力,在此测量中我们研究了机匣探针孔对边界层流场的干扰问题。灰尘油污的污染,气流温度随压气机工况的变化是遇到的主要问题。     

离心风机进出口三维流场的实验研究

文本将适用于单倾斜热线的周期多点采样技术和适用于五孔探针的集平均采样技术结合在一起,开发了一套适用于二者的数据采集和实时处理系统。该系统主要由探针(热线和五孔探针)、坐标架机构、采样同步脉冲发生系统、数据采集和转换系统、接口电路和 IBM 计算机组成。在 IBM 计算机的控制下,探针可由坐标架上的步进电机驱动作必要的转动和移动,采样同步脉冲启动 A/D 转换用以保证采样点的准确同步。利用该系统,成功地对离心风机叶轮进出口处的三维平均流场进行了测量,获得了叶轮进口无叶区的子午面速度分布和叶轮出口处的相对速度分布,并对试验获得的详细数据进行了分析。     

边界层综合诊断技术研究

给出了对二元翼型模型和三元三角翼模型表面边界层转捩用表面热膜技术、红外热像仪技术和液晶显示技术在同一风洞中同时进行显示和测量并进行比较的结果。对二元NACA-0012翼型表面边界层转捩点位置测量,三种方法都给出了相吻合的结果。三元的60°三角翼模型经过多次实验,测量结果表明表面热膜技术能够给出三角翼模型表面边界层转捩位置的定量侧量结果。红外热像仪技术和液晶显示技术研究在应用时受到环境条件的影响,在合适的条件下也能给出模型表面边界层转捩位置的定量结果。     

Effects of Low Energetic Neutral Atoms on Martian and Venusian Dayside Exospheric Temperature Estimations

The heating of the upper atmospheres and the formation of the ionospheres on Venus and Mars are mainly controlled by the solar X-ray and extreme ultraviolet (EUV) radiation (λ = 0.1–102.7 nm and can be characterized by the 10.7 cm solar radio flux). Previous estimations of the average Martian dayside exospheric temperature inferred from topside plasma scale heights, UV airglow and Lyman-α dayglow observations of up to ∼500 K imply a stronger dependence on solar activity than that found on Venus by the Pioneer Venus Orbiter (PVO) and Magellan spacecraft. However, this dependence appears to be inconsistent with exospheric temperatures (<250 K) inferred from aerobraking maneuvers of recent spacecraft like Mars Pathfinder, Mars Global Surveyor and Mars Odyssey during different solar activity periods and at different orbital locations of the planet. In a similar way, early Lyman-α dayglow and UV airglow observations by Venera 4, Mariner 5 and 10, and Venera 9–12 at Venus also suggested much higher exospheric temperatures of up to 1000 K as compared with the average dayside exospheric temperature of about 270 K inferred from neutral gas mass spectrometry data obtained by PVO. In order to compare Venus and Mars, we estimated the dayside exobase temperature of Venus by using electron density profiles obtained from the PVO radio science experiment during the solar cycle and found the Venusian temperature to vary between 250–300 K, being in reasonable agreement with the exospheric temperatures inferred from Magellan aerobraking data and PVO mass spectrometer measurements. The same method has been applied to Mars by studying the solar cycle variation of the ionospheric peak plasma density observed by Mars Global Surveyor during both solar minimum and maximum conditions, yielding a temperature range between 190–220 K. This result clearly indicates that the average Martian dayside temperature at the exobase does not exceed a value of about 240 K during high solar activity conditions and that the response of the upper atmosphere temperature on Mars to solar activity near the ionization maximum is essentially the same as on Venus. The reason for this discrepancy between exospheric temperature determinations from topside plasma scale heights and electron distributions near the ionospheric maximum seems to lie in the fact that thermal and photochemical equilibrium applies only at altitudes below 170 km, whereas topside scale heights are derived for much higher altitudes where they are modified by transport processes and where local thermodynamic equilibrium (LTE) conditions are violated. Moreover, from simulating the energy density distribution of photochemically produced moderately energetic H, C and O atoms, as well as CO molecules, we argue that exospheric temperatures inferred from Lyman-α dayglow and UV airglow observations result in too high values, because these particles, as well as energetic neutral atoms, transformed from solar wind protons into hydrogen atoms via charge exchange, may contribute to the observed planetary hot neutral gas coronae. Because the low exospheric temperatures inferred from neutral gas mass spectrometer and aerobraking data, as well as from CO⁺ ₂ UV doublet emissions near 180–260 nm obtained from the Mars Express SPICAM UV spectrograph suggest rather low heating efficiencies, some hitherto unidentified additional IR-cooling mechanism in the thermospheres of both Venus and Mars is likely to exist. An erratum to this article can be found at     

不同通道中气泡的形态变化及运动条件分析

孔隙是影响复合材料性能的主要因素之一,为了消除孔隙,提高产品质量,对复合材料成型过程中气泡运动特性的研究是十分必要的.利用预浸料片层模拟系统,考察了气泡在不同运动通道中穿出的形态变化过程;分析了外加压力、树脂粘度、气泡大小、网格面积等因素对气泡穿出行为的影响;同时提出了气泡穿出的约束条件.研究结果表明,随着树脂粘度的增加,气泡体积和空隙面积的减少,气泡穿出所需的临界压力将逐渐增大.该研究结果将为热压成型过程中气泡运动模型的建立提供实验依据.      

先驱体转化—热压烧结碳纤维增韧碳化硅复合材料的显微结构

采用ＸＲＤ,ＨＲＴＥＭ 和ＳＥＭ 等分析测试手段,研究了以聚碳硅烷（ＰＣＳ）为先驱体和粘结剂,Ｙ２Ｏ３ 和ＡｌＮ 为烧结助剂,采用先驱体转化－热压烧结法制备的Ｃｆ／ＳｉＣ复合材料的显微结构。结果表明,Ｙ２Ｏ３ 主要与ＰＣＳ的裂解产物以及ＡｌＮ 和ＳｉＣ表面的氧化物发生反应,形成有助于复合材料致密化的液相,而ＡｌＮ 则与烧结液相和ＰＣＳ之间通过反应－ 溶解－ 沉积过程,形成主要分布于界面相中的微小ＳｉＣ－ＡｌＮ 固溶体。正是由于含有一定量ＳｉＣ－ＡｌＮ 固溶体的富碳界面相使纤维与基体之间的结合适中,纤维易发挥脱粘和拔出作用,复合材料具有很好的力学性能     

随焊激冷对LY12CZ铝合金焊接热裂纹倾向影响的研究

采用自行研制的柔性接触式激冷器,分别以液氮和水作为冷却介质,研究了随焊激冷对ＬＹ１２ＣＺ铝合金焊接热裂纹率的影响。同时结合跨焊缝两侧横向位移的实时测量结果,分析了随焊激冷影响热裂纹率的作用机理。研究表明,采用随焊激冷工艺能够有效地降低ＬＹ１２ＣＺ铝合金的焊接热裂纹率,其原因在于随焊激冷显著增加了ＢＩＲ（脆性温度区间）内表观横向收缩量。