充液航天器大幅晃动耦合动力学建模仿真研究

针对充液航天器大幅液体晃动与全星姿态运动的耦合问题,文章采用三维质心面法建立了储箱级等效力学模型和全星级耦合姿态动力学方程。该方法将储箱内液体等效为只能在其质心面内运动的质心点,而液体晃动对储箱的作用力（含力矩）用质心点与质心面之间的相互作用来模拟,同时利用牛顿欧拉法推导了液体晃动与航天器姿态运动的耦合动力学方程。数值仿真表明,计算结果与其国外实验卫星的在轨测量结果基本一致,从而初步验证了质心面等效力学模型用于全星级大幅液体晃动耦合动力学分析的有效性。     

基于推力器的组合航天器质量特性辨识方法研究

组合航天器的质量特性辨识对提高其姿态轨道控制的精度和快速性有至关重要的作用。对基于推力器的总质量、质心位置和惯量矩阵的在轨辨识进行了研究。基于推力作用下的平动方程可得到质心位置和总质量的耦合辨识方程,基于转动方程可得到转动惯量和质心位置的耦合辨识方程,通过对角速度和线加速度进行多次采样,利用最小二乘法求解这2类辨识方程可完成总质量、质心位置和惯量矩阵的在轨辨识。基于上述辨识原理,提出一种闭环稳定的解耦质量特性辨识方法,通过设计合适的推力器工作策略,实现总质量、质心位置和惯量矩阵的解耦辨识,并采用一种不依赖于转动惯量的控制算法,使组合航天器的姿态在辨识结束后恢复到稳定状态。仿真表明,采用闭环稳定的解耦质量特性辨识方法,可保证组合航天器在推力器激励后的姿态稳定性。在仿真采用的动力学干扰、推力器误差和敏感器误差下,总质量、质心位置和惯量矩阵的辨识精度可达到10-3量级。     

采用双目视觉的非合作空间目标相对导航与惯性参数辨识方法

针对面向在轨服务的非合作空间目标测量感知问题，提出了一种基于双目视觉的相对导航与惯性参数辨识方法。利用目标表面的特征点建立几何坐标系，并分别设计了姿态测量和相对导航滤波器，实现了目标姿态、角速度、轨道，质心位置与惯量比的高精度估计。在此基础上，通过黏附卫星与非合作目标形成组合体，利用相对导航算法获得的质心位置和惯量比在黏附前后的变化，实现了目标质量和转动惯量的辨识。数值仿真试验证明了算法的有效性。     

六自由度气浮台及其姿态平台自动平衡系统设计

针对卫星交会对接中相对姿态和位置的控制问题,设计一种6自由度（DOF）气浮台,并推导出描述两个气浮台模拟卫星交会对接运动的耦合6自由度(DOF)动力学模型。为解决气浮台模拟空间失重环境中的重力力矩干扰问题,设计一种基于应用新颖的快速非奇异终端滑模面的自适应有限时间控制器的自动平衡系统,估计出质心位置,通过控制三个平衡质量块补偿姿态平台质心与旋转中心之间的位置偏差。李雅普诺夫理论推导和仿真结果表明,该方法可以快速完成对姿态平台质心位置的准确估计,实现质心与旋转中心的高度重合。     

对空间碎片的相对位姿估计

针对几何、质量特性参数均未知的空间碎片,提出一种基于扩展卡尔曼滤波（EKF）的相对位姿估计算法。该算法以单目相机获得的目标图像特征视线信息作为测量输入,以目标姿态、姿态角速度、惯量比、相对位置、相对速度和特征位置作为滤波状态。对算法进行可观性分析,给出两个可以保证算法可观性的条件。分别针对不同条件进行数值仿真,仿真结果表明新算法能够对几何和质量参数未知的空间碎片进行有效的相对位姿 估计。     

一种参数化非合作目标相对位姿和惯量估计方法

针对故障卫星、失效航天器、空间碎片等空间非合作目标无先验模型,且无法直接获得其角速度及惯量参数等问题,提出一种参数化非合作目标相对位姿和惯量参数估计方法。首先,基于自由航天器姿态动力学模型,用反双曲正切函数来描述含两个独立变量的惯量参数,建立非合作目标角速度传播模型方程;基于立体视觉测量模型,建立非合作目标上若干特征点的量测方程。然后,结合Clohessy-Wiltshire方程描述的航天器间相对运动学模型,以非合作目标的相对位置、相对线速度、相对姿态、惯性角速度及惯量参数为状态量,设计扩展卡尔曼滤波器以估计各状态量。最后,进行不同场景的数值仿真验证。蒙特卡洛仿真结果表明,所设计的滤波器在不同噪声水平下能够高精度地有效估计出非合作目标的相对位姿和惯量参数。     

旋转非合作目标相对状态的解耦估计方法

针对在轨旋转非合作目标相对状态估计中关于几何结构及惯量参数先验信息未知的问题，提出一种以双目相机对目标特征点的投影作为测量值的解耦估计方法，实现旋转非合作目标相对状态的估计。首先，建立非合目标的动力学模型和目标特征点的运动模型；其次，为避免由目标特征点与目标质心相对位置不确定引起滤波性能降低的问题，建立相对特征的运动模型及投影模型，对旋转运动和平移运动进行解耦；最后，设计相应的滤波器对非合作目标的相对状态进行估计。仿真结果表明，提出的解耦估计方法能够有效地估计出非合作目标的相对状态。     

一种星间相对状态估计方法

编队自主导航是实现分布式遥感系统星间协同观测的基础。为实现分布式遥感系统星间相对状态的精确确定，提出一种基于MEMS激光雷达与纳型星罗盘的星间相对状态估计方法。借助相对姿态、轨道运动学方程建立了星间相对状态的无迹卡尔曼滤波(UKF)算法，解决了MEMS激光雷达测量与参考航天器姿态耦合的问题，并利用预定入轨参数及高精度轨道外推(HPOP)对方法进行仿真校验。结果表明，该方法具有可行性和实用性，估计精度满足分布式遥感任务需求，能够较好解决中远距离星间相对状态估计问题。     

基于SoftPOSIT算法的单目视觉非合作目标相对位姿估计

针对模型尺寸已知的非合作目标,在目标三维特征点和图像二维特征点坐标已知但匹配关系未知的条件下,对基于SoftPOSIT算法的非合作目标航天器间相对位姿估计方法进行了研究。SoftPOSIT算法将解决匹配的Softassign和解决位姿的POSIT两种迭代方法融入一个迭代循环,建立全局目标函数,最小化目标函数就可在获得服务航天器与目标航天器相对位姿的同时确定三维点与二维点间的匹配关系。仿真结果表明由SoftPOSIT算法所得位态精度很高,算法正确有效。在不同条件下用该算法对某卫星位姿进行估计,发现算法的相对位置估计精度随目标与服务航天器相对距离增大而提高,而相对姿态角对估计精度的影响较小。     

一种非合作目标相对位置和姿态确定方法

针对非合作目标中的从星若无法获得主星的动态信息时,就无法自主进行相对位置和姿态确定的问题,提出了一种采用陀螺、立体视觉系统和加速度计的相对状态确定方法。首先分别建立相对姿态方程、主星动力学方程和相对位置方程等系统的数学模型。然后根据这些方程组成的状态方程和立体视觉系统的测量模型设计了卡尔曼滤波器。该滤波器使得从星根据加速度计、陀螺和立体视觉系统的输出,在仅获得主星的外观特征和一些静态参数的情况下,能够自主进行相对位置和姿态的确定。最后,数值仿真结果表明,在相同仿真条件下,与使用主星陀螺信息的相对状态确定算法相比,该算法能够自主进行相对状态的确定,且位置和姿态稳态误差分别为0.05m和2°。     

The motion of a synchronous satellite in a system similar to the earth-moon system

The stationary motions of a synchronous axisymmetric satellite are studied in the field of attraction by the Earth and a third body whose parameters are close to those of the Moon. Equations of motion are written in canonical variables that take into account the resonance character of the problem. The plots characterizing the dependence of the rotation parameters of the satellite relative to the center of mass on the elements of satellite’s translational motion are presented. A picture is given that represents the initial configuration of the system for implementing stationary motions.     

绳系卫星系统复杂模型研究

对绳系卫星系统提出一种仿真度更高的动力学模型，着重研究状态保持阶段的子星的振荡与姿态运动。主星设为质点，与系统质心相合，作圆轨道运动；子星取为三维刚体，系绳采用株式模型。除绳系统动能、引力位能及系绳弹性势能外，还考虑了系绳的结构阻尼，以及由系绳外皮包引起的弯曲力矩与扭转力矩。计算机辅助推导参与模拟计算程序设计。     

一种海洋测高卫星质心在轨估计算法

为了满足海洋测高卫星在轨质心位置精度的要求,提出了一种使用陀螺仪测量数据在轨估算卫星质心位置的算法。该算法利用推力器工作产生外力矩,采用总体最小二乘法,综合考虑了实际推力器推力的误差及陀螺仪的测量误差,由卫星的姿态动力学方程估算得到卫星质心位置。数值仿真证明了该算法的有效性,结果表明质心位置的估计精度在毫米量级,可以满足海洋测高卫星对质心位置精度的需求。     

Rapid rotations of a satellite with a cavity filled with viscous fluid under the action of moments of gravity and light pressure forces

Rapid rotational motion of a dynamically asymmetric satellite relative to the center of mass is studied. The satellite has a cavity filled with viscous fluid at low Reynolds numbers, and it moves under the action of moments of gravity and light pressure forces. Orbital motions with an arbitrary eccentricity are supposed to be specified. The system, obtained after averaging over the Euler-Poinsot motion and applying the modified averaging method, is analyzed. The numerical analysis in the general case is performed, and the analytical study in the axial rotation vicinity is carried out. The motion in the specific case of a dynamically symmetric satellite is considered.     

Translational–Rotational Motion of a Viscoelastic Sphere in Gravitational Field of an Attracting Center and a Satellite

We study the translational–rotational motion of a planet modeled by a viscoelastic sphere in the gravitational fields of an immovable attracting center and a satellite modeled as material points. The satellite and the planet move with respect to their common center of mass that, in turn, moves with respect to the attracting center. The exact system of equations of motion of the considered mechanical system is deduced from the D'Alembert–Lagrange variational principle. The method of separation of motions is applied to the obtained system of equations and an approximate system of ordinary differential equations is deduced which describes the translational–rotational motion of the planet and its satellite, taking into account the perturbations caused by elasticity and dissipation. An analysis of the deformed state of the viscoelastic planet under the action of gravitational forces and forces of inertia is carried out. It is demonstrated that in the steady-state motion, when energy dissipation vanishes, the planet's center of mass and the satellite move along circular orbits with respect to the attracting center, being located on a single line with it. The viscoelastic planet in its steady-state motion is immovable in the orbital frame of reference. It is demonstrated that this steady-state motion is unstable.     

冗余空间机械臂抓捕自旋卫星后的消旋控制

旨在提出一种运动学冗余空间机器人抓捕自旋卫星后的消旋策略和协调控制方法。首先，给出运动学冗余空间机器人捕获目标后的动力学模型，作为协调控制器设计基础。然后，基于四阶Bézier曲线和满足特定约束的自适应微分进化(Differential Evolution, DE)算法提出抓捕后的最优消旋与路径规划策略，最优消旋策略中同时考虑对消旋时间和控制力矩进行优化。提出一种跟踪所设计参考轨迹的协调控制方法，调整基座的姿态达到期望值。所提方法有效地衰减了自旋卫星的初始角速度，同时实现对基座姿态的控制。文末给出利用7 DOF冗余空间机械臂消除目标自旋运动的仿真结果，表明所提方法的有效性。     

Relative position and attitude estimation of spacecrafts based on dual quaternion for rendezvous and docking

The capacity to acquire the relative position and attitude information between the chaser and the target satellites in real time is one of the necessary prerequisites for the successful implementation of autonomous rendezvous and docking. This paper addresses a vision based relative position and attitude estimation algorithm for the final phase of spacecraft rendezvous and docking. By assuming that the images of feature points on the target satellite lie within the convex regions, the estimation of the relative position and attitude is converted into solving a convex optimization problem in which the dual quaternion method is employed to represent the rotational and translational transformation between the chaser body frame and the target body frame. Due to the point-to-region correspondence instead of the point-to-point correspondence is used, the proposed estimation algorithm shows good performance in robustness which is verified through computer simulations.     

On the stability of spinning satellites

We study the directional stability of rigid and deformable spinning satellites in terms of two attitude angles. The linearized attitude motion of a free system about an assumed uniform-spin reference solution leads to a generic MGK system when the satellite is rigid or deformable. In terms of Lyapunov’s stability theory, we investigate the stability with respect to a subset of the variables. For a rigid body, the MGK system is 6-dimensional, i.e., 3 rotational and 3 translational variables. When flexible parts are present the system can have any arbitrary dimension. The 2×2 McIntyre–Myiagi stability matrix gives sufficient conditions for the attitude stability. A further development of this method has led to the Equivalent Rigid Body method. We propose an alternative practical method to establish sufficiency conditions for directional stability by using the Frobenius–Schur reduction formula. As practical applications we discuss a spinning satellite augmented with a spring–mass system and a rigid body appended with two cables and tip masses. In practice, the attitude stability must also be investigated when the spinning satellite is subject to a constant axial thrust. The generic format becomes MGKN as the thrust is a follower force. For a perfectly aligned thrust along the spin axis, Lyapunov’s indirect method remains valid also when deformable parts are present. We illustrate this case with an apogee motor burn in the presence of slag. When the thrust is not on the spin axis or not pointing parallel to the spin axis, the uniform-spin reference motion does not exist and none of the previous methods is applicable. In this case, the linearization may be performed about the initial state. Even when the linearized system has bounded solutions, the non-linear system can be unstable in general. We illustrate this situation by an instability that actually happened in-flight during a station-keeping maneuver of ESA’s GEOS-I satellite in 1979.     

模糊神经网络控制器在卫星姿态控制系统中的应用

现代卫星的姿轨控制面临着挠性附件对本体姿态的耦合作用。本文将卫星太阳帆板挠性结构对本体姿态的影响增广进系统方程 ,在PID控制器控制刚体卫星的基础上 ,设计了模糊神经网络控制器 ,采用反向传播和最小方差估计的学习方法进行模糊规则的学习 ,仿真表明 ,模糊神经网络特有的学习和处理定性与定量知识的优点 ,将使卫星姿态在参数变化与外部干扰情况下具有较好的姿态稳定度与精度。