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.     

基于参数优化的脉冲轨道设计

基于参数优化设计了一种可处理各类脉冲轨道优化的一般方法,并给出了两种确定最优脉冲数的方法。以脉冲矢量与脉冲施加时刻为未知参数,将脉冲轨道优化设计转为非线性参数优化,用合适的非线性规划算法求解。主矢量理论对所得解最优性的验证表明该方法可行。     

轨道机动时考虑延迟的卫星姿态稳定控制方法

轨道机动时,测量与传输延迟,以及偏心推力对卫星姿态的持续扰动,造成传统的姿态稳定控制方法控制性能下降。为了克服这些问题,设计了对外扰与状态同时估计的闭环-开环预测器。在外扰力矩定常的假设下,给出了此种估计器对状态与外扰的预测都收敛的判定准则。利用估计出的外部扰动前馈补偿推力偏心干扰力矩,同时利用预测出的系统状态设计状态反馈控制器。通过求解两个代数Riccati方程,设计最优状态反馈增益和预测器增益。这种简单的前馈反馈结构具有良好的工程可实现性,同时仿真结果显示,该方法可以有效克服延迟和干扰的影响,提高卫星轨道机动时本体姿态稳定精度。
     

空间交会寻的最优轨道机动

研究了交会寻的阶段的燃料优化问题。在经典Ｃ－Ｗ方法基础上,导出了考虑第一次脉冲位置的双脉冲寻的燃料优化方法。当寻的时间给定时,优化变量为第一次脉冲启动的时刻;当寻的时间不定时,优化变量为第一次脉冲启动的时刻和寻的时间。仿真结果表明,考虑和不考虑第一次脉冲位置,燃料消耗差别悬殊。对于地面站较少、要求寻的时间比较长的情况,该方法有重要意义。     

近距离空间交会动力学

首先研究两个飞行器在近距离相对运动的动力学方程,包括简易（线性化）和精确模型;其次推导出一个工程实用在轨道平面内保持点轨迹椭圆方程;最后讨论保持点的动力学特性和轨道摄动对保持点的影响。     

Artificial equilibrium points and bi-impulsive maneuvers to observe 243 Ida

In the restricted three-body problem, the traditional Lagrange points L₁ and L₂ are the only equilibrium points near the asteroid 243 Ida. The thrust generated by a solar sail over a spacecraft enables the existence of new artificial equilibrium points, which depend on the position of the spacecraft with respect to the asteroid and the attitude of the solar sail. Such equilibrium points generate new spots to observe the body from above or below the plane of motion. Such points are very good observational locations due to their stationary condition. This work provides a preliminary analysis to observe Ida through the use of artificial equilibrium points as spots combined with transfer maneuvers between them. Such combination can be used to observe the asteroid from more different points of view in comparison to fixed ones. The analyses are made for a spacecraft equipped with a solar sail and capable of performing bi-impulsive maneuvers. The solar radiation pressure is used both to maintain the equilibrium condition and to reduce the costs of the transfers and/or to create transfers with longer duration. This is a new aspect of the present research, because it combines the continuous thrust with initial and final small impulses, which are feasible for most of the spacecraft, because the magnitudes of the impulses are very low. These combined maneuvers may reduce the transfer times of the maneuvers in most of the cases, compared with the maneuvers based only on continuous thrust. Several options involved in these transfers are shown, like to minimize the fuel spent ($\mathrm{\Delta }\mathit{v}$) as a function of the transfer time or to extend the duration of the travel between the points. Extended transfer times can be useful when observations are required during the transfers.     

空间机动目标的跟踪和定位

轨道机动控制过程中，推力加速度的不确定性是机动目标运动的主项摄动。通过对推力加速度和机动目标运动建模，在地心惯性系建立了增广系统状态动力学模型，在地平测量坐标系建立了离散量测模型，同时讨论了机动目标增广状态非线性动力学模型的线性化问题。给出了扩展卡尔曼滤波实时估计增广状态向量的算法，仿真分析证明所述算法稳定、收敛，对机动目标具有较高的定位精度。     

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.     

在轨加注用超声波流量计的设计与试验

针对航天器在轨加注对推进剂流量的精确测量要求,研制了在轨加注用超声波流量计。在对传播时间法研究的基础上,提出流量计管路布局的设计要求,采用计算流体动力学(Computational Fluid Dynamics, CFD)的方法模拟4种不同管路布局(直角型、45°锐角型、直线型和圆弧型)对流体速度分布的影响,对比得到了优化的管路布局。信号处理电路使用斩波稳定比较器,通过阈值比较法,保证了传播时间的测量精度。流量计经标定后,在量程（0～150g/s）范围内可达到0.1%的测量精度。为了验证在轨加注过程中流量计的作用,在地面环境下进行了在轨加注地面模拟试验,试验表明超声波流量计在推进剂在轨加注中使用是可行的和必要的。     

基于均匀圆形天线阵的涡旋电磁波产生与接收误差分析

为分析均匀圆形天线阵产生与接收涡旋电磁波时的误差特性,研究天线阵元激励相位存在高斯分布误差、量化误差以及单个阵元误差时产生的涡旋电磁波幅相特征,计算轨道角动量模态并给出准确辨认模态时的各误差阈值,分析接收阵列与产生阵列不平行时的幅相分布.仿真结果表明,在各类相位误差条件下,涡旋电磁波主瓣幅度由环状变得不规则,相位在主瓣宽度内保持良好,轨道角动量模态在小倾斜角接收误差下不能辨认.研究结果说明涡旋电磁波对各类激励相位误差具有良好的抗干扰特性,对倾斜角接收误差具有较高的敏感性,这将为利用涡旋电磁波实现多路复用奠定基础.