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。     

航空铝合金材料腐蚀裂纹扩展性能试验

腐蚀环境下的裂纹扩展性能是航空金属结构损伤容限设计的重要前提,为此,试验测定了3种航空铝合金材料(即2E12-T3、2E12-T42和7050-T7451)在2种腐蚀环境(3.5wt%NaCl溶液和油箱积水)下的裂纹扩展性能,在试验数据的基础上进行性能对比,并对试样断口进行SEM分析,研究了腐蚀和载荷联合作用对裂纹扩展的影响机理,研究结果表明:油箱积水环境对航空铝合金材料裂纹扩展的影响比3.5wt%NaCl溶液严重,铝合金2E12-T3和2E12-T42的腐蚀裂纹扩展性能优于铝合金7050-T7451,腐蚀环境下的氢脆效应和阳极溶解机制是造成腐蚀裂纹扩展加速的主要原因。     

飞机结构局部环境加速腐蚀当量谱

提出了编制海军飞机结构关键危险部位环境谱的技术途径,在地面停放环境谱的基础上,综合考虑关键部位的结构形式、密封性等诸多因素,给出局部环境谱。提出用金属腐蚀电流Ｉｃ作为度量尺度和用控制金属表面湿润时间的方法,对环境谱加速。经试验得出加速腐蚀折算系数α,将局部环境谱转换成给定环境下的当量加速试验谱。加速腐蚀损伤与机场环境损伤结果相吻合。     

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。     

推进剂贮箱用2A14铝合金接头应力腐蚀性能研究

为了研究推进剂贮箱用2A14铝合金接头介质相容性,分析了铝合金的应力腐蚀机理,以2A14-T6铝合金本体、搅拌摩擦焊(FSW)接头和变极性氩弧焊(VPTIG)接头为研究对象,通过慢应变速率拉伸法进行应力腐蚀试验研究。结果表明,2A14铝合金在3.5%NaCl溶液中存在应力腐蚀现象,FSW接头的抗腐蚀性能优于VPTIG接头。。     

高强度钢表面镀锌、镉层加速腐蚀试验研究

通过模拟海洋大气环境所设计的中性盐雾、加速盐雾、多因子复合3种加速腐蚀试验方法,考察了高强度钢表面镀锌、镉层的腐蚀性能与特点,并将实验室加速试验结果与厦门海洋大气腐蚀结果进行了相关性分析。研究结果表明:中性盐雾试验对镀锌层具有一定的加速腐蚀效应,对镀镉层的腐蚀则比较缓慢,而且与海洋大气环境的腐蚀结果相关性差;采用含有Cl^-,SO^2-₃,NO^-₃,SO^2-₄,pH等环境成分因子的加速盐雾试验,对镀镉、镀锌层具有较好的加速腐蚀效应,且镀锌层腐蚀结果与海洋大气环境腐蚀具有一定的相关性;多因子复合加速腐蚀试验方法将SO₂气氛、湿热、紫外线照射、加速盐雾等环境因子引入试验,明显加快了镀锌、镀镉层的腐蚀速度,且镀锌层腐蚀结果与海洋大气环境的腐蚀结果存在着对应的线性关系,线性相关系数为0.9889,与厦门外场腐蚀环境具有较好的相关性。     

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     

基于威布尔分布的C-T曲线通用性分析

为研究载荷谱、恒幅应力水平及裂纹尺寸对疲劳寿命预腐蚀影响系数C(T)的影响,建立了基于疲劳寿命服从威布尔分布的C(T)对比法.地面停放预腐蚀对结构疲劳寿命的影响规律可以用C-T曲线表示,当预腐蚀疲劳寿命位于长寿命段,常假定其服从威布尔分布,C(T)为预腐蚀后和未腐蚀结构特征寿命的比值.取预腐蚀疲劳寿命分布函数的形状参数为材料常数,采用极大似然方法估计特征寿命,得到其分布特性,从而建立了C(T)估计量的分布特性,构造了不同环境下的C(T)统计对比法,用于C-T曲线通用性分析. 试验数据分析表明,当取疲劳寿命服从威布尔分布时,C-T曲线与载荷谱、应力水平及裂纹尺寸基本无关.     

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.