绳系卫星横向振动的控制方法

研究绳系卫星绳索横向振动问题。首先建立绳索振动方程,由Pontrgasin方法求得抑制绳索横向振动的纵向优化控制力。实现方式为开启母星体内的电机控制绳长使星体产生加速度,星体惯性力导致绳轴向附加张力。      

磁带机运转对星载CCD相机成像的影响

利用Ｌａｇｒａｎｇｅ方程,建立了磁带轮转动和卫星姿态振动相互影响的仿真模型,并用数值计算方法计算了卫星的姿态振动,仿真分析了对星载线阵ＣＣＤ成像质量的影响。     

High precision and efficiency robotic milling of complex parts:Challenges,approaches and trends

Due to the advantages of large workspace, low cost and the integrated vision/force sensing, robotic milling has become an important way for machining of complex parts. In recent years,many scholars have studied the problems existing in the applications of robotic milling, and lots of results have been made in the dynamics, pose planning, deformation control etc., which provides theoretical guidance for high precision and high efficiency of robotic milling. From the perspective of complex parts r...     

模拟打伤/抛修缺口对TC17钛合金叶片振动疲劳性能的影响

研究了无缺口、打伤缺口和3种抛修缺口对TC17钛合金叶片振动疲劳性能的影响。结果表明,无缺口模拟叶片的疲劳寿命最长且寿命分散性最小,打伤缺口模拟叶片的疲劳寿命最短且寿命分散性最大,3种抛修缺口模拟叶片的疲劳寿命介于前两者之间,其中抛修缺口Ⅰ模拟叶片的疲劳寿命最长。无缺口和抛修缺口模拟叶片的疲劳裂纹均起源于叶片根部,打伤缺口模拟叶片的裂纹产生于缺口底部,与有限元模拟计算的最大应力位置吻合。模拟叶片的疲劳断裂区比较平坦,呈半椭圆形貌,疲劳源区主要位于模拟叶片表面的微小损伤处,疲劳扩展区具有典型的疲劳弧线特征,并呈现沿α/β片状组织界面开裂的特征。     

弹性高超声速飞行器建模及精细姿态控制

为保证超燃冲压发动机的良好进气,需要对高超声速飞行器进行精细姿态控制,但弹性振动问题极大影响其精细姿态控制精度。以高超声速飞行器的纵向通道为例,分析弹性振动问题对飞行控制系统的影响,建立面向控制的弹性高超声速飞行器数学模型,考虑气动参数和模态参数的大范围摄动,采用主动控制策略,基于鲁棒H∞理论和LQR理论设计精细姿态控制系统。大量仿真表明：在考虑测量噪声、舵机非线性、参数大范围摄动的情况下,控制系统能够很好地跟踪刚体攻角,抑制弹性攻角,并保证进气口当地攻角±0.4度的控制精度,满足高超声速飞行器精细姿态控制的要求。     

挠性航天器的鲁棒多目标姿态控制器设计

航天器挠性附件的振动难以直接测量且对航天器的姿态控制精度产生不利影响。为解决这一问题,提出一种基于观测器的鲁棒多目标姿态控制系统设计方法,借助特征结构配置的参数化方法,给出了含有自由参向量的控制器以及观测器的完整参数化形式。通过对自由参向量的多目标优化选取,使控制系统具有良好的鲁棒性和干扰抑制能力,并避免了控制输出饱和现象的发生。对一个挠性航天器的设计实例表明了方法的有效性。
     

大挠性空间桁架结构的动力学建模与仿真研究

对航天器结构中常用的一字型空间桁架,基于建立的普通式和拉索式空间桁架结构简化模型,用有限元法建立空间桁架结构模型,分别对两种空间桁架结构的模态特性、谐响应和瞬时激励响应等动力学特性进行了仿真研究,分析了拉索式空间桁架结构的弦张力对桁架结构振动特性的影响。研究较好地模拟了大挠性空间桁架结构的动力学特性及其在外太空的真实工况,有一定的参考意义。     

振动台动态角的测试方法研究

振动台在高频振动过程中难免会产生空间的小角度运动,这种角运动在振动试验中是非预期的,应尽量减小。利用激光干涉原理,运用双频激光干涉仪及角度测量组件测量了振动台振动频率达2 000Hz时方位、俯仰、横滚三个方向的实时角度、角速率。通过对测量数据的分析可知环境的振动对测量准确度影响较大,为进一步完善该测试方法指明了研究方向。     

Designing method of acceleration and deceleration control schedule for variable cycle engine

Studies show that different geometries of a Variable Cycle Engine (VCE) can be adjusted during the transient stage of the engine operation to improve the engine performance. However, this improvement increases the complexity of the acceleration and deceleration control schedule. In order to resolve this problem, the Transient-state Reverse Method (TRM) is established in the present study based on the Steady-state Reverse Method (SRM) and the Virtual Power Extraction Method (VPEM). The state factors in the component-based engine performance models are replaced by variable geometry parameters to establish the TRM for a double bypass VCE. Obtained results are compared with the conventional component-based model from different aspects, including the accuracy and the convergence rate. The TRM is then employed to optimize the control schedule of a VCE. Obtained results show that the accuracy and the convergence rate of the proposed method are consistent with that of the conventional model. On the other hand, it is found that the new-model-optimized control schedules reduce the acceleration and deceleration time by 45% and 54%, respectively. Meanwhile, the surge margin of compressors, fuel–air ratio and the turbine inlet temperature maintained are within the acceptable criteria. It is concluded that the proposed TRM is a powerful method to design the acceleration and deceleration control schedule of the VCE.     

Wolf–Rayet optically thick winds with Alfvén waves

The Wolf–Rayet (WR) stars are hot luminous objects which are suffering an extreme mass loss via a continuous stellar wind. The high values of mass loss rates and high terminal velocities of the WR stellar winds constitute a challenge to the theories of radiation driven winds. Several authors incorporated magnetic forces to the line driven mechanism in order to explain these characteristics of the wind. Observations indicate that the WR stellar winds may reach, at the photosphere, velocities of the order of the terminal values, which means that an important part of the wind acceleration occurs at the optically thick region. The aim of this study is to analyze a model in which the wind in a WR star begins to be accelerated in the optically thick part of the wind. We used as initial conditions stellar parameters taken from the literature and solved the energy, mass and momentum equations. We demonstrate that the acceleration only by radiative forces is prevented by the general behavior of the opacities. Combining radiative forces plus a flux of Alfvén waves, we found in the simulations a fast drop in the wind density profile which strongly reduces the extension of the optically thick region and the wind becomes optically thin too close its base. The understanding how the WR wind initiate is still an open issue.