有分布质量系绳的卫星系统的动力学

以一组偏微分方程建立起的数学模型和采用距离速率控制算法来描述系统的受控运动。创建的递推算法用于计算系统的定常运动和称驻形。根据求解小偏差运动方程和通过边界条件求解特征根以判定驻形的稳定性。给出了模拟结果。     

环件轧制参数与质量关系研究

在分析环件加工过程的运动和受力的基础上,定义了环件的端面平整度和外圆的圆度误差作为环件质量的表征参数。通过仿真,分析了环件轧制过程中芯辊进给速度、驱动辊转速和上锥辊进给速度与环件质量之间的关系。仿真结果为环件轧制工艺参数定义提供了参考。     

横风对涡环旋转伞系统运动的影响

涡环旋转伞是一种常见的旋转降落伞,下落运动过程受横风的影响严重。基于伞塔实验的高速摄影和图像处理技术,提取涡环旋转伞系统水平和竖直方向的弹道数据点,结合弹道模型,利用遗传算法对气动力参数进行识别。文章分析了横风对涡环旋转伞系统弹道特性的影响,结果表明:涡环旋转伞的轴向力系数为1.02,大于一般其他类型伞;涡环旋转伞系统在横风作用下能很快达到稳定;横风对系统运动轨迹的影响较大,对落速和转速的影响较小。     

车载卫星天线用交流伺服系统设计

为实现在运动车辆上收看卫星电视，设计了车载卫星天线用交流伺服系统。给出了方案的基本原理，并采用矢量控制对交流电机进行变频调速，以及位置、速度和电流反馈的三闭环调节器。确定了电流环、速度环和位置环的参数。仿真结果表明，所设计的交流伺服系统有良好的动态和抗干扰性能。     

五轴相贯线焊接机器人控制系统研究

提出了一种以PMAC运动控制器为控制系统核心的五轴相贯线焊接机器人运动算法,分析了机器人的轨迹规划,对机器人的控制系统进行了相关研究.通过建立五轴相贯线焊接机器人的空间运动模型,推导出了相应的运动方程.确定了五轴相贯线焊接机器人系统的控制方案,研究了控制环的调整及参数选择,对控制及系统精度、误差补偿进行了一些理论分析.     

绳系卫星系统二维平面运动和常规动力学

在假设了无质量的系绳和地球中心引力场后，绳系卫星系统在同一轨道平面内运动由子星－母星之间相对位置向量描述，亦即由该向量的长度（两星间距）变化和方位角的变化而决定。在引入距离速率控制算法之后，系统的动力学主要由方位角运动而定。当母星轨道为圆形时，系统运动状态具有极限点，而在椭圆轨道下则有极限环。采用了非线性动态系统的方法和技术来计算极限状态和分析它们的稳定特性以及运动的分形问题。用本文中方法对ＴＳＳ     

环柱式天线展开过程耦合动力学分析

针对环柱式天线展开过程中斜拉绳索释放运动与桁架展开运动之间耦合动力学分析困难的问题,采用非线性欧拉梁单元对斜拉绳索建模,基于几何精确梁理论对环形桁架建模,提出了环柱式天线多体系统模型,实现了结构展开过程中绳索释放与桁架展开耦合动力学的精准仿真,揭示了绳索柔性等因素对桁架伸展起阻碍作用的机理。仿真结果表明,在环柱式天线展开过程中,减小绳索模量,降低绳索直径,采用单绳索分布设计,有利于提高桁架的展开稳定性。另外,绳索柔性对桁架展开中间阶段影响最为显著。该分析结果为环柱式天线在轨展开动力学预示和优化设计提供了指导作用。     

单通道控制旋转弹系统动力学建模与Hopf分岔

为准确预测旋转弹系统的锥形运动形态并判断其稳定性，提出一对鸭舵引起的气动不对称性以及可能引起复杂非线性动力学特性的非线性因素，建立能准确描述单通道控制旋转弹系统姿态运动的复数形式的动力学模型并分析讨论其动态稳定性条件。利用分岔理论对单通道控制旋转弹系统开展Hopf分岔研究，给出了Hopf分岔发生的判断准则；推导了用于判定极限环稳定的第一Lyapunov系数。数值仿真结果验证了条件的正确性与有效性并发现了拟周期运动及混沌运动。研究结果为旋转弹的控制参数设计及结构参数设计提供理论参考。     

高空零压气球上升过程的运动特性研究

飞行在20km～100km高度的临近空间浮空器,在区域监视、侦查、应急通信与科学实验等领域具有独特的优势。高空零压气球是常见的临近空间浮空平台之一。对其上升过程运动特性的研究有利于增加驻空时间、减少横向漂移距离。文章通过建立零压气球充气量模型和气球上升过程中的动力学模型,对气球上升过程中动力学模型进行仿真分析,结合高空飞行试验数据,验证了所建模型的准确性。在模型的基础上对比了不同浮升气体对气球上升速度以及驻空高度的影响;研究了浮升气体充气量对载荷总量的影响,并分析了气球在上升过程中的体积变化以及驻空高度与浮升气体质量的关系,最后讨论了影响气球上升特性的关键因素。可以得到零压气球上升过程运动特性与浮升气体种类、充入气体量、气球规格、载荷质量有关,假设气球可无限膨胀不发生爆炸,浮升气体密度越小,充入气体量越多,载荷质量越轻,气球的驻空高度就越高,达平衡所需时间越少;实际工程应用中,气球受材料限制不可无限膨胀,面密度小的气球,可能在上升到驻空高度前发生爆炸,要使气球携带一定质量载荷在某一高度范围驻空,其充气量不能过多,需与一些物理量满足一定关系。     

在嫦娥一号探月工程中求定月球重力场问题的探讨

月球重力场制约着近月外空间物体的运动，同时环月飞行器的运动也反映了月球重力场的作用。本文结合我国嫦娥一号探月工程，探讨了利用月球卫星地面跟踪资料，求定月球重力场的基本理论和方法，分析了环月卫星的轨道高度、地面跟踪采样时间间隔和跟踪精度等对月球重力场求定的影响。     

TETHERED SATELLITE SYSTEM ANALYSIS (1) — TWO-DIMENSIONAL CASE AND REGULAR DYNAMICS

The study on tethered satellite system (TSS) in two-dimensional in-planar motion is restricted in that the tether is assumed to be massless. The equations of motion are given in a spherical coordinate system to describe the magnitude (tether length) and direction angle of the position vector between the satellites. A length rate control algorithm is adopted, and the controlled motion of the directional angle by the algorithm will have a stable equilibrium state. The equilibrium state is a fixed point if the orbit of the base-satellite is circular, and a limit cycle if the orbit is elliptic. The value and stability of the equilibrium state are determined by the parameters of the control algorithm, and the bifurcation analysis is also given. Two typical TSS missions have been simulated.     

基于三阶解析解的小行星平衡点附近halo轨道确定方法研究

尽管周期解的存在性已经被证明,但要在给定的动力学系统中寻找到满足一定精度要求的周期解依然是一件极富挑战性的工作.提出如下方法确定小行星平衡点附近精确的周期轨道(halo轨道).首先扩展运动方程:将小行星平衡点附近轨道运动方程的右端项在平衡点处展成三阶幂级数.从而将非线性运动学方程扩展为拟线性微分方程.然后求近似解析解:应用Lindstedt-Poincaré方法求解扩展后的运动方程组,将周期解和其运动频率展开成三阶幂级数,并将二者代人扩展后的拟线性微分方程中.这样就可以得到三个不同阶的线性运动方程,逐次求解三个微分方程并消除解中的永年项即可得到hal.轨道的三阶解析解.最后微分校正:将周期轨道在三阶解析解附近线性化,得到状态转移矩阵,并使用状态转移矩阵和轨道终端状态的偏差修正轨道初值,从而得到满足精度要求的精确引力场中的halo轨道.     

Variation of the Satellite Orbit Altitude by the Light Pressure Force

The possibility of the uncontrolled increase of the altitude of an almost circular satellite orbit by the force of the light pressure is investigated. The satellite is equipped with a damper and a system of mirrors (solar batteries can serve as such a system). The flight of the satellite takes place in the mode of a single-axis gravitational orientation, the axis of its minimum principal central moment of inertia makes a small angle with the local vertical and the motion of the satellite around this axis constitutes forced oscillations under the impact of the moment of force of the light pressure. The form of the oscillations and the initial orbit are chosen so that the transverse component of the force of the light pressure acting upon the satellite be positive and the semimajor axis of the orbit would continuously increase. As this takes place, the orbit remains almost circular. We investigate the evolution of the orbit over an extended time interval by the method which employs separate integration of the equations of the orbital and rotational motions of the satellite. The method includes outer and inner cycles. The outer cycle involves the numerical integration of the averaged equations of motion of the satellite center of mass. The inner cycle serves to calculate the right-hand sides of these equations. It amounts to constructing an asymptotically stable periodic motion of the satellite in the mode of a single-axis gravitational orientation for current values of the orbit elements and to averaging the equations of the orbital motion along it. It is demonstrated that the monotone increase of the semimajor axis takes place during the first 15 years of motion. In actuality, the semimajor axis oscillates with a period of about 60 years. The eccentricity and inclination of the orbit remain close to their initial values.     

Radial velocity search for low mass companions of nearby stars

The detection of substellar companions of nearby stars is very difficult, because these objects are very faint and are located close to their bright parent stars. One way to attack this problem is to look for small periodic motion of the bright star, induced by the gravitational attraction exerted by the unseen small companion. Over the past decade stellar spectroscopy has been used by a few teams to monitor the radial velocities of several samples of stars, with a threshold for detection of companions well below the substellar limit of about 0.08 M. So far, only a few possible spectroscopic binaries have been identified where the unseen companions might be substellar.Recently, radio observers discovered that the millisecond pulsar PSR B1257+12 displays periodic variations in the pulse arrival times, indicating the existence of at least three unseen companions in circular orbits around the pulsar. This is the first convincing case for an extra-solar planetary system. This discovery suggests that planetary systems can form in very different situations, and therefore may prove to be common.     

Periodic motions of a satellite-gyrostat relative to its center of mass under the action of gravitational torque

We investigated periodic motions of the axis of symmetry of a model satellite of the Earth, which are similar to the motions of the longitudinal axes of the Mir orbital station in 1999–2001 and the Foton-M3 satellite in 2007. The motions of these spacecraft represented weakly disturbed regular Euler precession with the angular momentum vector of motion relative to the center of mass close to the orbital plane. The direction of this vector during the motion was not practically changed. The model satellite represents an axisymmetric gyrostat with gyrostatic moment directed along the axis of symmetry. The satellite moves in a circular orbit and undergoes the action of the gravitational torque. The motion of the axis of symmetry of this satellite relative to the absolute space is described by fourth-order differential equations with periodic coefficients. The periodic solutions to this system with special symmetry properties are constructed using analytical and numerical methods.     

Revisiting the general periodic relative motion in elliptic reference orbits

A general periodicity condition is presented by analyzing the relative motion between two spacecraft performing formation flight in Keplerian elliptic orbits. The Tschauner–Hempel equation is used to describe the relative motion, and the general periodicity condition is derived through a state transition matrix with a true anomaly as a free variable. The general periodicity condition is also derived by using the energy matching condition, and the resulting periodic conditions by two approaches are compared to each other. Moreover, the zero offset condition is presented to locate the leader spacecraft at the center of the formation geometry. Then, the periodic relative motion in the elliptic reference orbit is expressed using the periodicity condition and the zero offset condition. Numerical simulations demonstrate the periodic relative motion in the elliptic reference orbit, and the results show that the general periodicity condition guarantees the bounded periodic relative motion in arbitrary elliptic orbits, and the zero offset condition makes the formation center coincide with the leader spacecraft.     

Periodic motions of a nearly dynamically symmetric satellite in the neighborhood of hyperboloidal precession

The motion of a satellite close to a dynamically symmetric solid body in a Newtonian gravitational field over a circular orbit is studied. The system of differential equations describing the body’s motion is close to a system with cyclic coordinate. New classes of periodic motions are constructed in the neighborhood of a known partial solution to an unperturbed problem, hyperboloidal precession of a dynamically symmetric satellite. In the resonance case, when the ratio of one frequency of small oscillations of a reduced system with two degrees of freedom in the neighborhood of a stable equilibrium position to the frequency of cyclic coordinate variation is close to an integer number, there exist one or three families of periodic motions that are analytic in terms of fractional powers of a small parameter. A study of stability of these motions was performed with the help of KAM (Kolmogorov-Arnold-Moser) theoty. Faling the described resonance there exists a unique family of periodic motions that is analytic in terms of integer powers of a small parameter. The check-up of stability of these motrons was carried out. We distinguished the cases of parametric resonance, resonances of the third and fourth orders, and a non-resonant case. In the resonance cases our study relies on well-known results on stability of Hamiltonian systems during resonances [1]. In the non-resonant case we use the KAM theory [2].     

Solar sail formation flying on an inclined Earth orbit

The versatility of solar sail propulsion can be utilized in the exploration of Earth’s magnetotail. An inclined periodic orbit with respect to ecliptic is possible for a solar sail with its orbital plane in synchronous rotation with the sun. Solar sail evolving on such an inclined orbit is free of Earth shadow. Formation flying of a cluster of sails around such an inclined periodic orbit is investigated in this paper. The solution of the first-order approximation to the linear relative motion is used to qualitatively analyze the configurations of relative orbits. Since the relative motion is unstable, active control is necessary to keep a periodic relative motion. A typical LQR method is employed to stabilize the relative motion. The design method is validated by numerical examples.     

基于T-H方程的卫星轨迹模型参考输出跟踪控制方法

当目标卫星沿椭圆轨道运行时,描述追踪星与目标星相对运动的线性化方程为T-H方程。将描述航天器相对运动的T-H方程变换为周期系统的状态空间形式,并给出卫星轨迹跟踪控制问题的数学描述。基于周期系统的参量Lyapunov方法和模型参考跟踪控制理论,提出了卫星轨迹跟踪控制器的设计方法。利用该方法设计了带有收敛速率保障的反馈镇定控制器和具有自由参数的前馈控制器。对追踪星相对目标星悬停任务进行了数值仿真,仿真结果表明提出的控制方案是有效的。