陀螺进动与强迫进动轨道

陀螺进动与轨道进动现象的相似性归因于二者的动力学相似性. 通过类比二者的动力学模型,提出了一类强迫进动轨道. 若以圆轨道为初始轨道,通过施加常值法向力可以实现一种特殊的悬浮型强迫进动轨道. 采用四元数建模方法求解了这种强迫进动轨道的进动规律,给出了解析表达式,据此分析了这种轨道的性质. 分析结果表明这种强迫进动轨道与初始圆轨道在同一球面上,且与初始位置相切. 其角速度为进动角速度与初始轨道角速度的合成,是一种悬浮轨道,即属于非开普勒轨道. 悬浮轨道在地球观测、行星际科学、天文观测、无线电通讯以及地球工程等领域具有潜在应用前景. 从强迫进动的角度出发所作的分析为悬浮轨道的实现提供了一种新途径.     

卫星编队飞行中相对轨道的J2摄动分析

详细分析了$J_{2}$摄动对编队卫星相对轨道构形的影响. $J_{2}$ 摄动对相对轨道的影响分为相对轨道构形的漂移、相对轨道平面的章动和进动. 首先, 分析了相对轨道构形漂移速度、章动角速度和进动角速度的一阶近似表达式的数量级及其影 响因素. 其次,给出一个准则,来判断同一相对轨道的漂移和转动之间的关系. 最后, 利用该准则,分析了主、从星的轨道根数差对相对轨道的漂移和转动的影响.     

Displaced orbits generated by solar sails for the hyperbolic and degenerated cases

Displaced non-Keplerian orbits above planetary bodies can be achieved by orientating the solar sail normal to the sun line. The dynamical systems techniques are employed to analyze the nonlinear dynamics of a displaced orbit and different topologies of equilibria are yielded from the basic configurations of Hill’s region, which have a saddlenode bifurcation point at the degenerated case. The solar sail near hyperbolic or degenerated equilibrium is quite unstable. Therefore, a controller preserving Hamiltonian structure is presented to stabilize the solar sail near hyperbolic or degenerated equilibrium, and to generate the stable Lissajous orbits that stay stable inside the stabilizing region of the controller. The main contribution of this paper is that the controller preserving Hamiltonian structure not only changes the instability of the equilibrium, but also makes the modified elliptic equilibrium become unique for the controlled system. The allocation law of the controller on the sail’s attitude and lightness number is obtained, which verifies that the controller is realizable.     

USEFUL RELATIVE MOTION DESCRIPTION METHOD FOR PERTURBATIONS ANALYSIS IN SATELLITE FORMATION FLYING

Nomenclature OXYZEarth’sequatorialinertialreferenceframeωArgumentofperigee SlxyzLeadingsatelliteorbitframeMMeananomaly SfxyzFollowingsatelliteorbitframefTrueanomalyaSemi majoraxisθ=ω fArgumentoflatitude eEccentricitynMeanmotion iOrbitinclinationrSatel…     

Solution set on the natural satellite formation orbits under first-order earth＇s non-spherical perturbation

Using the reference orbital element approach, the precise governing equations for the relative motion of formation flight are formulated. A number of ideal formations with respect to an elliptic orbit can be designed based on the relative motion analysis from the equations. The features of the oscillating reference orbital elements are studied by using the perturbation theory. The changes in the relative orbit under perturbation are divided into three categories, termed scale enlargement, drift and distortion respectively. By properly choosing the initial mean orbital elements for the leader and follower satellites, the deviations from originally regular formation orbit caused by the perturbation can be suppressed. Thereby the natural formation is set up. It behaves either like non-disturbed or need little control to maintain. The presented reference orbital element approach highlights the kinematics properties of the relative motion and is convenient to incorporate the results of perturbation analysis on orbital elements. This method of formation design has advantages over other methods in seeking natural formation and in initializing formation.     

Sensitivity analysis for a type of statically stable sailcrafts

Two types of sensitivities are proposed for statically stable sailcrafts.One type is the sensitivities of solar-radiation-pressure force with respect to position of the center of mass,and the other type is the sensitivities of solar-radiation-pressure force with respect to attitude.The two types of sensitivities represent how the solar-radiationpressure force changes with the position of mass center and the attitude.Sailcrafts with larger sensitivities undergo larger error of the solar-radiation-pressure force,leading to larger orbit error,as demonstrated by simulation.Then as a case study,detailed formulas are derived to calculate the sensitivities for sailcrafts with four triangular sails.According to these formulas,in order to reduce both types of sensitivities,the angle between opposed sails should not be too large,and the center of mass should be as close to the axis of symmetry of the four sails as possible and as far away from the center of pressure of the sailcraft as possible.     

A METHOD TO CORRECT CATALOG ORBIT DETERMINATION VELOCITY 1)

对于大批量空间目标,监测资源有限,测轨数据稀疏,导致编目定轨结果误差较大。本文分析了不同轨道类型的编目轨道预报误差演化特性,分析结果表明,轨道预报误差主要分布在沿迹方向,且主要是由于大气阻力摄动模型误差和初始径向速度误差引起的。进一步的理论推导显示,在忽略初始位置误差的假设条件下,轨道初值误差引起的预报位置误差前后具有近似对称特性,利用仿真数据,验证了近似对称特性的正确性。基于上述分析,本文提出了一种校准编目定轨初始速度的方法,即通过减小向前预报的位置与已知位置的偏差来迭代地校准定轨结果的速度,从而提高目标向后预报的轨道精度。利用实际轨道数据的试验结果表明,该方法对于采用稀疏数据的近圆轨道目标定轨结果修正效果明显,可以有效改进自主编目定轨结果的精度,对提高大批量空间目标的编目管理能力具有重要价值。     

Near-Earth asteroid flyby trajectories from the Sun-Earth L2 for Chang’e-2’s extended flight

Driven by curiosity about possible flight options for the Chang'e-2 spacecraft after it remains at the Sun-Earth L2 point, effective approaches were developed for designing preliminary fuel-optimal near-Earth asteroid flyby trajectories. The approaches include the use of modified unstable manifolds, grid search of the manifolds' parameters, and a two-impulse maneuver for orbital phase matching and z-axis bias change, and are demonstrated to be effective in asteroid target screening and trajectory optimization. Asteroid flybys are expected to be within a distance of 2×107 km from the Earth owing to the constrained Earth-spacecraft communication range. In this case, the spacecraft's orbital motion is significantly affected by the gravities of both the Sun and the Earth, and therefore, the concept of the "heliocentric oscillating-Kepler orbit" is proposed, because the classical orbital elements of the flyby trajectories referenced in the heliocentric inertial frame oscillate significantly with respect to time. The analysis and results presented in this study show that, among the asteroids whose orbits are the most accurately predicted, "Toutatis", "2005 NZ6", or "2010 CL19" might be encountered by Chang'e-2 in late 2012 or 2013 with total impulses less than 100m/s.     

WHY CAN THE MAJOR PLANETS HAVE THEIR SATELLITES MOVING IN DIRECT AND RETROGRADE ORBITS AS WELL?

Now we use the Jacobian integral of circular restricted three-body problem toestablish a testing function of the stability of satellites.This method of criterion may beapplied to the stability problem of satellites when the six elements of the instantaneous orbitof the satellite with respect to its parent planet are known.By means of an electronic computer,we can find the stable region of a satellite with aquasi-circular orbit.The boundary surface of this region is a nearly oblate ellipsoid.Thevolume of this enclosed space is much smaller than that of binding by Hill surface and thatof“sphere of action”.As the expressions of relative kinetic energy of a satellite with respect to its parentplanet have the same form for the direct as well as the retrograde orbits,they can coexist inthe same region at the same time.     

HOVERING ORBITS DESIGN FOR PERTURBED ASTEROIDS WITH PARAMETRIC EXCITATION RESONANCE 1)

本文将太阳引力摄动视为受摄不规则小行星系统的组成部分,借鉴非线性振动理论中参数激励共振的概念,创新性地设计了不规则小行星平衡点附近稳定的悬停观测轨道.为了同时考虑不规则小行星引力和太阳引力, 本文采用受摄粒杆模型描述系统.通过对未扰系统平衡点以及固有频率的分析, 给出系统存在参激共振轨道的条件.再以第二类参激主共振和1:3内共振为例,采用多尺度方法求得参数激励共振轨道的稳态解, 并对稳态解的稳定性进行判断.通过受摄小行星系统的幅频响应曲线以及力频响应曲线分析了系统的非线性特性以及参数激励效应.此外, 对内共振引起的长短周期能量转移现象进行了分析.本文的研究成果可以拓展现有小行星系统周期轨道族设计方法.     

<Emphasis Type="Italic">J</Emphasis><Subscript>2</Subscript> invariant relative orbits via differential correction algorithm

This paper describes a practical method for finding the invariant orbits in J ₂ relative dynamics. Working with the Hamiltonian model of the relative motion including the J ₂ perturbation, the effective differential correction algorithm for finding periodic orbits in three-body problem is extended to formation flying of Earth’s orbiters. Rather than using orbital elements, the analysis is done directly in physical space, which makes a direct connection with physical requirements. The asymptotic behavior of the invariant orbit is indicated by its stable and unstable manifolds. The period of the relative orbits is proved numerically to be slightly different from the ascending node period of the leader satellite, and a preliminary explanation for this phenomenon is presented. Then the compatibility between J ₂ invariant orbit and desired relative geometry is considered, and the design procedure for the initial values of the compatible configuration is proposed. The influences of measure errors on the invariant orbit are also investigated by the Monte–Carlo simulation. The project supported by the Innovation Foundation of Beihang University for Ph.D. Graduates, and the National Natural Science Foundation of China (60535010).     

火星引力捕获动力学与动态误差分析

火星探测的制动捕获机会唯一,是影响任务成败的关键. 从限制性三体问题出发,推导了火星引力球、作用球与希尔球半径的计算公式,比较了三者的特点与适用范围,并结合作用球的定义与物理意义,给出了一种火星探测制动捕获段的工程定义. 在作用球范围内建立了火星制动捕获段动力学模型,给出了对捕获轨道精度产生影响的各项误差源. 通过蒙特卡洛仿真,定量分析了导航初始误差、发动机推力误差、制动点火时间误差等对捕获轨道近火点与远火点高度的影响,并对不同误差源可能导致的超差概率进行了分析,指出了影响捕获精度的主导误差源,可为我国未来火星探测制动捕获段的任务实施提供参考.      

A method for classifying orbits near asteroids

A method for classifying orbits near asteroids under a polyhedral gravitational field is presented, and may serve as a valuable reference for spacecraft orbit design for asteroid exploration. The orbital dynamics near aster- oids are very complex. According to the variation in orbit characteristics after being affected by gravitational perturbation during the periapsis passage, orbits near an as- teroid can be classified into 9 categories： （1） surrounding- to-surrounding, （2） surrounding-to-surface, （3） surrounding- to-infinity, （4） infinity-to-infinity, （5） infinity-to-surface, （6） infinity-to-surrounding, （7） surface-to-surface, （8） surface- to-surrounding, and （9） surface-to- infinity. Assume that the orbital elements are constant near the periapsis, the gravitation potential is expanded into a harmonic series. Then, the influence of the gravitational perturbation on the orbit is studied analytically. The styles of orbits are dependent on the argument of periapsis, the periapsis radius, and the periapsis velocity. Given the argument of periapsis, the orbital energy before and after perturbation can be derived according to the periapsis radius and the periapsis velocity. Simulations have been performed for orbits in the gravitational field of 216 Kleopatra. The numerical results are well consistent with analytic predictions.     

气动力辅助变轨的数值模拟

采用了航天器在行星上层大气中进行高超声速飞行时的轨道动力学方程,针对航天器从地球静止轨道转移到一个共面圆形低地轨道的变轨过程,进行了气动力辅助变轨过程的模拟.在变轨过程中,航天器从地球静止轨道开始,经过8次大气路径,耗时43.7小时,到达圆形低地轨道,与霍曼转移进行对比,其所消耗的推进剂质量仅为霍曼转移的41%.研究结果表明:气动力辅助变轨技术能够在降低推进剂消耗的情况下实现航天器的轨道转移.     

Optimal control of a spacecraft with a solar sail

Analysis of the results indicates that:

近圆参考轨道卫星编队洛仑兹力控制

基于运动电荷在磁场中切割磁力线受到洛仑兹力作用的物理规律,分析了两种带电模式对经典轨道根数长期变化的影响:(1)卫星恒定带电模式;(2)前半个轨道周期卫星带电、后半周期不带电的非恒定带电模式.恒定带电模式可以有效地改变轨道升交点赤经、近地点幅角以及平近点角,对轨道半长轴、偏心率和倾角几乎不产生长期影响;而非恒定带电模式则可以有效地改变轨道偏心率.基于洛仑兹力作用下轨道根数长期变化规律以及轨道根数差描述的带电副星相对于不带电主星的运动,提出了利用洛仑兹力以及两种带电模式实现地球低轨近圆参考轨道卫星编队的控制策略,包括编队绕飞椭圆大小重构与编队中心漂移控制,解析求解了副星所需的带电量,并利用数值仿真验证了洛仑兹力控制的可行性.需要指出的是,洛仑兹力轨道控制无需消耗推进工质.      

Dynamics in large generators due to oval rotor and triangular stator shape

Earlier measurements in large synchronous generators indicate the existence of complex whirling motion, and also deviations of shape in both the rotor and the stator. These non-symmetric geometries produce an attraction force between the rotor and the stator,called unbalanced magnetic pull(UMP).The target of this paper is to analyse responses due to certain deviations of shape in the rotor and the stator.In particular,the perturbation on the rotor is considered to be of oval character,and the perturbations of the stator are considered triangular.By numerical and analytical methods it is concluded for which generator parameters harmful conditions,such as complicated whirling motion and high amplitudes,will occur.During maintenance of hydro power generators the shapes of the rotor and stator are frequently measured.The results from this paper can be used to evaluate such measurements and to explain the existence of complex whirling motion.     

THE CONTROL OF MEGA-CONSTELLATION AT LOW EARTH ORBIT BASED ON TLE

近几年来,美国SpaceX, OneWeb等创新型企业纷纷计划打造低轨巨型卫星星座,引发卫星互联网的发展热潮。本文利用公开的两行轨道根数(two-line element, TLE)对国外星座控制策略进行分析,重点分析了铱星、一网、星链星座的控制规律。通过相对相位偏差分析,反演得到星座中不同卫星之间的平半长轴差,避免了小控制量条件下难以通过平半长轴判断卫星是否进行了轨控的问题。获得了国外星座控制频次和控制精度等重要信息,所得结论能够为我国未来互联网星座的建设提供参考。     

Averaging analyses for spacecraft orbital motions around asteroids

This paper summarizes a few cases of spacecraft orbital motion around asteroid for which averaging method can be applied, i.e., when central body rotates slowly, fast, and when a spacecraft is near to the resonant orbits between the spacecraft mean motion and the central body＇s rotation. Averaging conditions for these cases are given. As a major extension, a few classes of near resonant orbits are analyzed by the averaging method. Then some resulted conclusions of these averaging analyses are applied to understand the stabil- ity regions in a numerical experiment. Some stability conclu- sions are obtained. As a typical example, it is shown in detail that near circular 1 ： 2 resonant orbit is always unstable.     

Orbit and attitude control of spacecraft formation flying

Formation flying is a novel concept of distributing the functionality of large spacecraft among several smaller, less expensive, cooperative satellites. Some applications require that a controllable satellite keeps relative position and attitude to observe a specific surface of another satellite among the cluster. Specially, the target space vehicle is malfunctioning. The present paper focuses on the problem that how to control a chaser satellite to fly around an out-of-work target satellite closely in earth orbit and to track a specific surface. Relative attitude and first approximate relative orbital dynamics equations are presented. Control strategy is derived based on feedback linearization and Lyapunov theory of stability. Further, considering the uncertainty of inertia, an adaptive control method is developed to obtain the correct inertial ratio. The numerical simulation is given to verify the validity of proposed control scheme.