叶片掠对跨声转子进口流动的影响

选择NASA Rotor 37跨声转子作为原型叶片,在叶片90%展高以上通过移动叶型基元的弦向位置构造叶尖掠特征,共有包括原型转子、2个前掠转子和2个后掠转子等5种不同叶型几何的算例.利用数值模拟软件计算得到5种转子的总体特性并获得三维流场.结果表明:叶尖前掠减小了叶片尖部进口的平均攻角,而后掠则使攻角增大.引入周向平均无黏动量方程,计算出由周向平均所产生的周向不均匀源项及径向平衡方程的各项数值,并对比其在5个转子进口的分布规律及其与攻角变化之间的关联.通过改变进口的流动平衡,叶尖前掠使轴向速度增大、周向速度减小,进而使得攻角减小;后掠则在叶尖起到了相反的效应.采用这种准三维方法研究了叶片掠对叶片进口流场的影响.      

航天器轨道控制系统的智能设计方法与仿真

本文介绍了将智能控制方法用于航天器交会对接段的轨道控制。通过建立系统的特征模型、知识库、数据库和规则库并且构造出相应的推理机构和控制逻辑,为航天器的轨道控制过程设计了一种专家式智能控制器。仿真结果表明了此系统具有较好的跟踪性能。     

有限推力下相对绕飞轨道的直接形成

提出了一种有限推力下主动航天器在完成轨道转移的同时形成相对目标航天器绕飞的方法。根据以改进春分点轨道根数表示的非奇异轨道摄动方程,用变分方法将问题转化为经典的最优控制,由相对运动动力学获得主动航天器实现绕飞须满足的终端约束条件,再用非线性规划求解。给出了求解模型。理论分析和仿真结果表明,该方法理论上可行,但为减少干扰产生的偏差,还需对绕飞形成过程中的导引率进行研究。     

行星齿轮箱耦合调制振动信号分离与故障诊断

针对故障状态下行星齿轮箱振动信号通常表现为稳态调制和冲击调制成分耦合问题,建立不同求解模型,提出耦合调制振动信号分离方法。应用稀疏全变分模型实现冲击调制成分分离,采用改进的非对称惩罚函数,根据峭度系数与方均根系数指标构建正则化参数优选策略,采用受控极小化(majorization-minimization, MM)方法进行模型求解;采用基追踪实现稳态调制成分分离。试验结果分析表明:该方法在噪声D为0.15的信号中能快速分离出微弱冲击调制成分,算法迭代次数少、收敛效果好。      

无人机制造外形气动偏差评估方法

气动外形对无人机起着至关重要的作用,有必要对其制造外形的气动偏差进行评估。利用数字摄影测量系统获得无人机制造外形的点云数据;以机头为参考点,将测量点云数据模型与理论模型的坐标系重合,对比重合度并统计无人机制造外形与理论外形的几何偏差分布;根据点云数据进行逆向建模,获得无人机制造外形的三维模型;对无人机理论外形进行CFD计算,与其风洞试验数据进行对比,通过调整网格及计算方法,得到与试验数据相吻合的CFD计算方法;以此方法计算得到无人机制造外形的气动数据,并与无人机的理论气动力进行对比。结果表明:此评估方法能够定量地评估外形制造偏差对无人机气动特性的影响。     

基于图像化变差函数的性能数据异常明别

为提升发动机性能监控的智能化水平,实现性能数据的高效利用,提出了基于图像化变差函数的发动机性能数据异常 判别方法。 通过研究发动机性能数据的标准化修正方法和图像转化方法,将数值型表示的发动机性能数据转化为发动机性能图像。 通过引入变差函数理论,采用 4 方向的变差函数值表示性能特征值,融合不同时刻不同参数的性能数据。 在提取发动机性能图像关 键特征点的基础上,定义性能图像间的差异距离,实现基于变差函数的发动机性能图像异常判别方法,从而实现对发动机性能状态 的判别。 选用若干组实际发动机性能数据对方法进行验证O 验证结果表明:该方法运算高效,实现了高维性能数据的降维和对性能 图像运行状态的分类,从而判别发动机性能数据的运行状态。     

基于流场/声爆耦合伴随方程的超声速公务机声爆优化

基于自主研发的大规模并行结构化网格CFD求解器PMB3D以及并行化伴随方程求解器PADJ3D,开展了流场/声爆伴随方程的求解研究。首先采用标准算例,对内部CFD代码PMB3D软件和声爆预测代码进行了声爆计算可信度验证,以及声爆强度对近场声压梯度的校核。针对并行环境下多块对接网格的近场声压提取操作的复杂性,提出了包围盒的方法实现并行环境下近场声压装配单元编号、网格块编号以及对应的进程编号确定,基于声爆计算坐标将并行传递的数据进行一维排序,为声爆预测、伴随方程以及梯度求解提供输入条件。通过线性插值雅克比矩阵实现均匀坐标系梯度信息向非均匀坐标转换,并进一步根据结构化网格特征提出了插值原则,简化了近场声压转换雅克比矩阵的变分。通过装配单元记录,实现声爆强度对流场守恒变量的变分结果向各个进程装配,将装配结果作为流场伴随方程的右端项实现流场声爆耦合伴随方程的求解。此外,对小型超声速公务机开展了声爆优化,对比分析了设计前后的声压及其频谱特性。     

天波超视距雷达的发展

 天波超视距雷达 (OTHR)是一种利用电离层对高频信号的反射作用自上而下进行目标探测的雷达体制。由于该雷达具有大范围的监视能力、防低空突袭、抗隐身以及早期预警等突出优点 ,受到了许多国家的重视。首先介绍了OTHR的性能特点及发展历史 ,接着就雷达的总体结构、干扰的抑制、由电离层引起的信号失真的校正 ,以及信号检测进行了全面的综述 ,最后指出这一领域今后的发展方向。     

Effects of space weather on the ionosphere and LEO satellites’ orbital trajectory in equatorial,low and middle latitude

We study the effects of space weather on the ionosphere and low Earth orbit (LEO) satellites’ orbital trajectory in equatorial, low- and mid-latitude (EQL, LLT and MLT) regions during (and around) the notable storms of October/November, 2003. We briefly review space weather effects on the thermosphere and ionosphere to demonstrate that such effects are also latitude-dependent and well established. Following the review we simulate the trend in variation of satellite’s orbital radius (r), mean height (h) and orbit decay rate (ODR) during 15 October–14 November 2003 in EQL, LLT and MLT. Nominal atmospheric drag on LEO satellite is usually enhanced by space weather or solar-induced variations in thermospheric temperature and density profile. To separate nominal orbit decay from solar-induced accelerated orbit decay, we compute $r\text{,}h$ and ODR in three regimes viz. (i) excluding solar indices (or effect), where $r=r_0\text{,}h=h_0$ and $\mathit{ODR}={\mathit{ODR}}_0$ (ii) with mean value of solar indices for the interval, where $r=r_m\text{,}h=h_m$ and $\mathit{ODR}={\mathit{ODR}}_m$ and (iii) with actual daily values of solar indices for the interval ($r\text{,}h$ and ODR). For a typical LEO satellite at h?=?450?km, we show that the total decay in r during the period is about 4.20?km, 3.90?km and 3.20?km in EQL, LLT and MLT respectively; the respective nominal decay ($r_0$) is 0.40?km, 0.34?km and 0.22?km, while solar-induced orbital decay ($r_m$) is about 3.80?km, 3.55?km and 2.95?km. h also varied in like manner. The respective nominal ${\mathit{ODR}}_0$ is about 13.5?m/day, 11.2?m/day and 7.2?m/day, while solar-induced ${\mathit{ODR}}_m$ is about 124.3?m/day, 116.9?m/day and 97.3?m/day. We also show that severe geomagnetic storms can increase ODR by up to 117% (from daily mean value). However, the extent of space weather effects on LEO Satellite’s trajectory significantly depends on the ballistic co-efficient and orbit of the satellite, and phase of solar cycles, intensity and duration of driving (or influencing) solar event.     

Mapping orbits around the asteroid 2001SN263

The present paper has the goal of mapping orbits, with respect to the perturbations, for a spacecraft traveling around the asteroid 2001SN₂₆₃. This asteroid is a triple system, which center of mass is in an elliptic orbit around the Sun. The perturbations considered in the present model are the ones due to the oblateness of the central body, the gravity field of the two satellite bodies (Beta and Gamma), the Sun, the Moon, the asteroids Vesta, Pallas and Ceres and all the planets of the Solar System. This mapping is important, because it shows the relative importance of each force for a given orbit for the spacecraft, helping to make a decision about which forces need to be included in the model for a given accuracy and nominal orbit. Another important application of this type of mapping is to find orbits that are less perturbed, since it is expected that those orbits have good potential to require a smaller number of station-keeping maneuvers. Simulations under different conditions are made to find those orbits. The main reason to study those trajectories is that, currently, there are several institutions in Brazil studying the possibility to make a mission to send a spacecraft to this asteroid (the so-called ASTER mission), because there are many important scientific studies that can be performed in that system. The results showed that Gamma is the main perturbing body, followed by Beta (10 times smaller) and the group Sun–Mars-oblateness of Alpha, with perturbations 1000 times weaker than the effects of Gamma. The other bodies have perturbations 10⁷ times smaller. The results also showed that circular and polar orbits are less perturbed, when compared to elliptical and equatorial orbits. Regarding the semi-major axis, an internal orbit is the best choice, followed by a larger external orbit. The inclination of the orbit plays an important role, and there are values for the inclination where the perturbations show minimum and maximum values, so it is important to make a good decision on those values.