基于碳纳米管薄膜的复合材料在线损伤监测

考虑到纤维增强树脂基复合材料会在服役过程中因受冲击、压缩以及疲劳等因素的作用而发生损伤,基于碳纳米管薄膜优异的力电响应特性开发了一种具有在线损伤监测能力的自感知复合材料。碳纳米管可在薄膜中形成导电网络,复合材料损伤会破坏导电通路,使碳纳米管薄膜的电阻大幅度增加。通过测量自感知复合材料的边界电压并利用电阻层析成像法对碳纳米管薄膜内电导率的分布变化进行求解/成像,实现了复合材料的在线损伤监测。分别对贯穿孔损伤和I型层间断裂损伤模式进行了研究,结果表明所制备的自感知复合材料对这两种损伤模式均可实现损伤定位及图像化显示,对于贯穿孔型损伤模式可实现对面积占比0.038%的损伤进行在线监测,定位精度可达毫米级。     

新型航空发动机空气冷却器流动传热性能试验

空气冷却器是航空发动机中空气热量交换的重要场所,针对传统扰动结构强化换热不足问题,重点研究了空气冷却器 中扰动结构的结构形貌特征与流动换热的关系。以三周期极小曲面结构为基础,设计制造了D型极小曲面扰动结构、P型极小曲 面扰动结构和基于Sigmoid函数杂化方法的D-P型（P-D型）结构。并利用纳米CT重构出样品的3维数字特征,试验研究了不同结 构来流速度与压降、换热性能和综合换热性能的关系。结果表明：D型极小曲面结构具有最优的压降、换热性能和综合换热性能： D-P型杂化极小曲面结构的阻力系数f最大,比D型结构的高56.81%;D型的平均努塞尔数Nu比P型的高18.49%,P-D和D-P杂 化结构的换热性能比P型结构的有效提高;P-D型D-P型杂化结构的Nu分别比P型结构的高2%和8.27%。在4种结构中,D型结 构的综合换热性能最优,分别比P型、P-D型、D-P型结构的高40.35%、57.2%、71.02%。     

Adaptive control and stabilization of elastic spacecraft

This work treats the question of large angle rotational maneuver and stabilization of an elastic spacecraft (spacecraft-beam-tip body configuration). It is assumed that the parameters of the system are completely unknown. An adaptive control law is derived for the rotational maneuver of the spacecraft. Using the adaptive controller, asymptotically decoupled control of the pitch angle of the space vehicle is accomplished, however this maneuver causes elastic deformation of the beam connecting the orbiter and tip body. For the stabilization of the zero dynamics (flexible dynamics), a stabilizer is designed using elastic mode velocity feedback. In the closed-loop system including the adaptive controller and the stabilizer, reference pitch angle trajectory tracking and vibration suppression are accomplished. Simulation results are presented to show the maneuver capability of the control system     

Interplanetary origin of geomagnetic storms

Around solar maximum, the dominant interplanetary phenomena causing intense magnetic storms (Dst<−100 nT) are the interplanetary manifestations of fast coronal mass ejections (CMEs). Two interplanetary structures are important for the development of storms, involving intense southward IMFs: the sheath region just behind the forward shock, and the CME ejecta itself. Whereas the initial phase of a storm is caused by the increase in plasma ram pressure associated with the increase in density and speed at and behind the shock (accompanied by a sudden impulse [SI] at Earth), the storm main phase is due to southward IMFs. If the fields are southward in both of the sheath and solar ejecta, two-step main phase storms can result and the storm intensity can be higher. The storm recovery phase begins when the IMF turns less southward, with delays of ≈1–2 hours, and has typically a decay time of 10 hours. For CMEs involving clouds the intensity of the core magnetic field and the amplitude of the speed of the cloud seems to be related, with a tendency that clouds which move at higher speeds also posses higher core magnetic field strengths, thus both contributing to the development of intense storms since those two parameters are important factors in genering the solar wind-magnetosphere coupling via the reconnection process. During solar minimum, high speed streams from coronal holes dominate the interplanetary medium activity. The high-density, low-speed streams associated with the heliospheric current sheet (HCS) plasma impinging upon the Earth's magnetosphere cause positive Dst values (storm initial phases if followed by main phases). In the absence of shocks, SIs are infrequent during this phase of the solar cycle. High-field regions called Corotating Interaction Regions (CIRs) are mainly created by the fast stream (emanating from a coronal hole) interaction with the HCS plasma sheet. However, because the B_z component is typically highly fluctuating within the CIRs, the main phases of the resultant magnetic storms typically have highly irregular profiles and are weaker. Storm recovery phases during this phase of the solar cycle are also quite different in that they can last from many days to weeks. The southward magnetic field (B_s) component of Alfvén waves in the high speed stream proper cause intermittent reconnection, intermittent substorm activity, and sporadic injections of plasma sheet energy into the outer portion of the ring current, prolonging its final decay to quiet day values. This continuous auroral activity is called High Intensity Long Duration Continuous AE Activity (HILDCAAs). Possible interplanetary mechanisms for the creation of very intense magnetic storms are discussed. We examine the effects of a combination of a long-duration southward sheath magnetic field, followed by a magnetic cloud B_s event. We also consider the effects of interplanetary shock events on the sheath plasma. Examination of profiles of very intense storms from 1957 to the present indicate that double, and sometimes triple, IMF B_s events are important causes of such events. We also discuss evidence that magnetic clouds with very intense core magnetic fields tend to have large velocities, thus implying large amplitude interplanetary electric fields that can drive very intense storms. Finally, we argue that a combination of complex interplanetary structures, involving in rare occasions the interplanetary manifestations of subsequent CMEs, can lead to extremely intense storms. This revised version was published online in June 2006 with corrections to the Cover Date.     

一种用于飞机试验台的三分力传感器

多分力载荷传感器是一种常用的传感器,但通常当各分力的量程相差太大时难以取得良好的效果。提出了一种新型传感器结构形式,减少了各分力之间的耦合,使得在各分力量程不匹配的情况下亦可获得较高的测量精度。     

外缘轴向进气的旋转空腔主盘局部换热及流阻特性研究

某型发动机的实际涡轮盘腔冷却结构被简化成外缘轴向进气的旋转空腔模型,以实验方法研究了旋转雷诺数(Re_ω)、冷气雷诺数Re_z)、哥拉晓夫数(Gr*)对主盘局部换热及流阻特性的影响。实验发现,冷气雷诺数、哥拉晓夫数的增大,使主盘局部换热系数在盘缘附近迅速增大,而在接近盘心时出现负值。阻力系数随旋转雷诺数的增大而减小,随冷气雷诺数的增大而增大。      

Beagle 2: a proposed exobiology lander for ESA's 2003 Mars Express mission.

The aim of the proposed Beagle 2 small lander for ESA's 2003 Mars Express mission is to search for organic material on and below the surface of Mars and to study the inorganic chemistry and mineralogy of the landing site. The lander will have a total mass of 60kg including entry, descent, and landing system. Experiments will be deployed on the surface using a robotic arm. It will use a mechanical mole and grinder to obtain samples from below the surface, under rocks, and inside rocks. Sample analysis by a mass spectrometer will include isotopic analysis. An optical microscope, an X-ray spectrometer and a Mossbauer spectrometer will conduct in-situ rock studies.     

减法消除CCD太阳Hα图象干涉条纹的误差分析

本文简要介绍了CCD产生干涉条纹的原因,对采用减法消除干涉条纹方法进行了论述。通过试验研究,提出了一种计算误差的方法,并对计算结果进行了分析和讨论。      

VHF/UHF振幅闪烁和VHF快速法拉弟旋转起伏

本文利用1988年9月至1989年5月在武昌(114.4°E,30.6°N)同时接收日本ETS-Ⅱ卫星(130.0°E)发出的VHF(136MHz)信标信号和苏联静止站-T卫星(99.0°E)发出的UHP(714MHz)广播电视信号时获得的观测记录,对夜间出现的双频(VHF/UHF)闪烁和VHF快速(每分钟大于5次的起伏)法拉弟旋转起伏(以下用FRF表示法拉弟旋转起伏)进行了统计分析,结果发现在临近太阳黑子最大年份观测到的双频夜间闪烁主要为急始型,呈赤道特性,且在临近二分点的月份里有最大出现率,秋季更为明显;伴随VHF振幅闪烁出现的快速FRF常与UHF振幅闪烁共存,以及产生这种现象的不规则体由西向东漂移,东-西向的漂移速度分量,在子夜前为140m/s,在子夜后为90m/s。