嫦娥五号探测器推进系统研制与飞行

本文介绍了嫦娥五号探测器推进系统的任务特点、研制要求、设计方案、主要单机技术以及在轨飞行表现。嫦娥五号推进系统由三部分组成：轨道器推进子系统、着陆器推进子系统、上升器推进子系统,均采用氦气恒压挤压式双组元统一推进系统。为实现探测器的目标,推进系统在以往技术基础上开发了一系列新技术和新产品,大幅减轻了系统干质量、提高了相关性能,并采取了一系列技术加强了产品可靠性和月面环境适应性,最终圆满实现了探测器的任务目标。     

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.     

Coronal Heating by Magnetic Explosions

From magnetic fields and coronal heating observed in flares, active regions, quiet regions, and coronal holes, we propose that exploding sheared core magnetic fields are the drivers of most of the dynamics and heating of the solar atmosphere, ranging from the largest and most powerful coronal mass ejections and flares, to the vigorous microflaring and coronal heating in active regions, to a multitude of fine-scale explosive events in the magnetic network, driving microflares, spicules, global coronal heating, and, consequently, the solar wind. This revised version was published online in June 2006 with corrections to the Cover Date.     

基于实验复模态参数的有限元模型修正

提出了一种利用非完备实验复模态参数,修正带有非比例阻尼矩阵结构有限元模型的迭代修正方法。首先,对处理困难的阻尼矩阵表达为质量与刚度矩阵的多项式组合,并给出了物理解释,被修正参数为该多项式的系数和结构的某些局部几何、材料参数,其修正结构物理意义明确,与结构的动态设计相适应,实例表明了本文修正方法的有效性。     

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.     

起落架双腔缓冲器初始压力的优化设计

本文提出并讨论了起落架双腔缓冲器的初始压力优化设计问题,给出了分析模型与方法。国产某运输机起落架改双腔的算例表明,该模型与方法是可行的。     

偏置动量系统中的挠性天线指向控制研究

从工程实践角度,探讨了在目前广泛采用的偏置动量轮三轴姿态稳定卫星上,进行大尺寸（３～５ｍ）和高指向精度（０．０５°）的挠性天性指向控制问题。在建立具有挠性天线的星体动力学模型,以及在借鉴和改进有关抑制挠性天线振动研究的基础上,设计了三轴稳定卫星平台上的挠性天线指向控制系统的方案。最后,根据数值仿真结果,给出了影响挠性天线指向精度的主要因素。     

利用前缘旋转控制边条翼外翼分离

边条翼在边条较小时中等迎角以上外翼就会出现分离,现提出用转动前缘表面来控制边条翼外翼分离。通过测力、油流和烟丝实验研究了转动前缘对机翼气动特性的影响。结果表明,在这种机翼上转动前缘对控制分离是有效的,升力增量最大可达３０％。可以预期,转动前缘与边条的综合作用,机翼的分离特性将有较大的改善     

保证试验对陶瓷试件疲劳强度的影响

 应用断裂力学理论分析了保证试验对陶瓷试件造成的损伤及其对疲劳强度的影响。保证试验后试件的最低强度可根据材料的亚临界裂纹扩展参量、保证应力和保证试验的卸载速率估算。采用惰性试验环境和高的卸载速率可获得较高的试件最低剩余强度值。     

大型固体火箭发动机喷管故障诊断的流场计算

针对某大型固体火箭发动机的喷管喉道后烧穿的故障进行了数值模拟,运用ＴＶＤ（ＴｏｔａｌＶａｒｉａｔｉｏｎＤｉｍｉｎｉｓｈｉｎｇ）ＭａｃＣｏｒｍａｃｋ格式求解了喷管内流场的二维轴对称Ｎ－Ｓ方程,获得了流场的详细结构图谱,分析了故障的成因,指出喷管型面的导数不连续会导致当地壁温升高,是引发故障的直接原因。