热膜温度效应研究

用热膜测模型表面摩擦应力,在风洞试验中已得到广泛的应用,但在飞行试验中,由于大气温度与地面温度有很大差异,因此传统的校准方法无法应用。本文通过对热膜的传热机理进行分析,找到一种温度修正方法。此方法用于飞行试验中,得到较好的结果。     

在(工作)持续时间短暂设备中伴随有燃烧的气体动力模型试验方法的特点

对在高焓、持续工作时间短暂设备中进行伴有燃烧过程的气体动力模型的试验方法的特点作了介绍。根据俄罗斯科学院西伯利亚分院理论及应用研究所组织这种试验工作所积累的经验 ,描述了解决各种各类与燃烧有关的问题的模型配备 ;在发动机进气道中的推力空气动力特性、压力及热通量的测量结果等等。由此说明试验时间为 50～ 2 0 0ms的热射式风洞是解决燃烧问题的可靠设备     

矢量二元收扩喷管热射流复杂流场特征研究

提出了一种二元收 扩矢量喷管的概念 ,用热射流实验台对二元矢量喷管进行了过膨胀状态下的喷管模型热态实验。测量了喷管壁面静压和喷管出口总压分布 ,用红外热成像技术给出了二元喷管热射流流场的清晰画面 ,并对流场特征进行了描述和分析。研究表明 ,在非设计状态 ,二元喷管管内有明显的流动分离现象 ,喷口射流总压严重畸变 ,在热射流流场中 ,射流流场呈现双势核结构。     

圆棒热挤压过程研究

用抛物面速度场,对圆棒热挤压过程进行上限分析。经理论计算和有关试验数据比较,所求得的挤压力具有足够高的精度;并利用所建立的数学模型对挤压过程死区、最佳模角和挤压力进行了系统地研究。     

定向凝固Rene125合金热裂倾向性研究

采用半定量等级评定方法，对定向凝固高温合金Ｒｅｎｅ１２５热裂倾向性进行了研究。试验结果表明，本文提出的热裂倾向性半定量等级评定方法具有较好的重复性；炉膛温度、浇注温度和壳型抽拉速率等定向凝固工艺参数对Ｒｅｎｅ１２５合金的热裂倾向性有明显的影响。     

热线风速计测量中污染误差的消除方法

 热线风速计和其它接触式测量方法比较,具有探针对流场干扰小,空时分辨力高,频响快等优点。它和激光风速计（非接触式）一起,已成为当前研究流动微观机理的主要测试技术。但它的应用范围却受测试环境洁净度的限制。当然,热线应尽量用于洁净的环境,但在某些场合很难保证流场中没有轻微的污染,这就引入了热线测量的污染误差——利用热线预校     

一种高硅镍铜合金高温热压缩变形的研究

利用Gleeble-1500热模拟材料实验机,对高硅镍铜合金铸态试样分别在温度为T1,T2,T3,T4,应变速率为S1,S2,S3,S4,S5时进行压缩变形.对该合金的高温塑性变形行为和热压缩后的组织演变规律进行了研究.分析了流变应力与应变速率和温度的关系,计算出了应力指数和变形激活能.结果表明,流变应力随应变速率的增加而增加,随温度的升高而减小,并且该合金在高温变形条件下发生动态再结晶.     

镍掺杂对α-Al2O3烧结过程、微观结构及力学性能的影响

 首先采用非均相沉淀包裹法制备金属镍包裹α-Al₂O₃复合微球粉体,然后采用热压烧结制备了Al₂O₃/Ni金属陶瓷。通过X射线衍射仪（XRD）、扫描电子显微镜（SEM）、能谱仪（EDS）对复合粉体及热压烧结产物的成分和结构进行了表征,利用阿基米德法测量了复合陶瓷的密度,分别通过三点弯曲法和单边切口横梁法对陶瓷试条的抗弯强度和断裂韧性进行评估。研究发现：金属镍的引入活化了α-Al₂O₃的烧结,镍粒子均匀地分布在氧化铝的晶界上,增加了弱界面,提高了氧化铝的断裂韧性,最高可达7.62 MPa·m^1/2。     

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     

CVD纤维及其增强金属基复合材料强度的分布特征研究

采用单一Weibull统计分布函数来描述CVD纤维抗拉强度的分散性,发现具有不同断裂机制的缺陷所引发的断裂其拉伸强度分布分别符合Weibull分布,并具有各自独特的形态和参数;对热压复合前后的纤维的抗拉强度分布特征进行分析比较,结果表明热压复合过程对纤维的性能及抗拉强度分布特征有一定的影响,这主要是因为热压改变了纤维内部缺陷的类型和分布。另外还就以上研究结论在纤维的生产及其产品的性能表征方法、纤维增强金属基复合材料性能的非破坏性评估方法上的应用进行了讨论。