Cassini Radio Science

Cassini radio science investigations will be conducted both during the cruise (gravitational wave and conjunction experiments) and the Saturnian tour of the mission (atmospheric and ionospheric occultations, ring occultations, determinations of masses and gravity fields). New technologies in the construction of the instrument, which consists of a portion on-board the spacecraft and another portion on the ground, including the use of the Ka-band signal in addition to that of the S- and X-bands, open opportunities for important discoveries in each of the above scientific areas, due to increased accuracy, resolution, sensitivity, and dynamic range.This revised version was published online in July 2005 with a corrected cover date.     

一种构造群组综合判断矩阵的方法

本文提出了一种如何构造判断矩阵的最优方法，从而可以有效地保证在层次分析法中所得判断矩阵的一致性。     

含中介轴承内圈局部缺陷的双转子系统的组合共振特性

针对航空发动机双转子系统建立简化的动力学模型,在考虑中介轴承非线性Hertz接触力和径向游隙等非线性因素的情况下,将中介轴承内圈局部缺陷模拟成倒置的等腰梯形凹槽,利用4阶Runge-Kutta法进行数值计算,得到系统的分岔图,并着重分析分岔区域的组合共振特性,结果表明：相较于无故障系统,该系统在分岔图上出现三个新的分岔区域,前两个分岔区域是由内圈故障特征频率与高低压转子的转频形成的组合频率诱发的组合共振引起的,第三个是由内圈故障特征频率诱发共振引起的,在分岔区域内,系统运动的周期性的变化规律表现为从近似单周期运动到概周期运动再到近似单周期运动。     

A statistical study of post-flare-associated CME events

We present a statistical study of post-flare-associated CMEs (PFA-CMEs) during the period from 1996 to 2010. By investigating all CMEs and X-ray flares, respectively, in the LASCO and GOES archives, we found 15875 CMEs of which masses are well measured and 25112 X-ray flares of which positions are determined from their optical counterparts. Under certain temporal and spatial criteria of these CMEs and solar flare events, 291PFA-CMEs events have been selected. Linking the flare fluxes with CME speeds of these paired events, we found that there is a reasonable positive linear relation between the CME linear speed and associated flare flux. The results show also the CME width increases as the flux of its associated solar flare increases. Besides we found that there is a fine positive linear relation between the CME mass and its width. Matching the flare fluxes with CME masses of these paired events, we find the CME mass increases as the flux of its associated solar flare increases. Finally we find the PFA-CME events are in regular more decelerated than the other CMEs.     

超模式斜采样遥感图像超分辨复原方法

超模式斜采样成像技术通过将两排探测器阵列倾斜成像提高相机空间分辨率。由于不满足香农采样定理．图像中出现混叠。为了降低混叠对遥感图像超分辨复原的影响,文章提出了一种结合最佳倒易晶胞的超分辨复原方法。该方法根据超模式斜采样频域对偶网格建立相应的混叠模型．通过权重函数衡量噪声和混叠在频谱中的分布,得到噪声、混叠最小最佳倒易晶胞;并基于Huber—MRF（Markov Random Field）图像先验模型建立了耦合最佳倒易晶胞的MAP（Maximuma Posterior）超分辨复原模型。实验表明,该方法降低了超模式斜采样成像中混叠对复原的影响,获得了良好的超分辨复原效果。     

基于MAP估计和广义高斯MRF的SAR图像边缘比率检测方法

SAR图像极低的信噪比以及乘性噪声给SAR图像的边缘检测带来了较大的困难。提出了一种针对SAR图像边缘的自适应贝叶斯检测方法。该方法利用广义高斯马尔可夫随机场作为局部均值的先验概率分布模型,利用贝叶斯准则推导了局部均值的最大后验概率估计。广义高斯马尔可夫随机场模型参数估计和局部均值估计采用联合迭代技术进行求解。边缘检测器的参数采用接收机操作性能曲线和卡方检验进行选择。基于实测SAR数据的仿真实验结果表明,本文的边缘检测算子是有效的,并优于已有的SAR图像边缘检测算子。     

Formation control using μ-synthesis for Inner-Formation Gravity Measurement Satellite System

Inner-Formation Gravity Measurement Satellite System (IFGMSS) is used to map the gravity field of Earth. The IFGMSS consists of two satellites in which one is called “inner satellite” and the other one is named as “outer satellite”. To measure the pure Earth gravity, the inner satellite is located in the cavity of the outer satellite. Because of the shield effect of the cavity, the inner satellite is affected only by the gravitational force, so it can sense Earth gravity precisely. To avoid the collision between the inner satellite and the outer satellite, it is best to perform a real-time control on the outer satellite. In orbit, the mass of the outer satellite decreases with the consumption of its propellant. The orbit angular rate of the inner satellite varies with time due to various disturbing forces. These two parameters’ uncertainties make the C–W function be not so accurate to describe the formation behavior of these two satellites. Furthermore, the thrusters also have some uncertainties due to the unmodelled dynamics. To cancel the effects caused by the above uncertainties, we have studied the robust control method based on the μ-synthesis. This μ-synthesis eliminates the conservativeness and improves the control efficiency comparing with the H_∞ method. Finally, to test the control method, we simulate an IFGMSS mission in which the satellite runs in a sun synchronous circular orbit with an altitude of 300 km. The simulation results show the effectiveness of the robust control method. The performances of the closed-loop system with the μ-controller are tested by the μ-analysis. It has found that the nominal performance, the robust stability and the robust performance are all achieved. The transient simulation results further prove the control response is fast and the accuracy of the relative position meets the demand of the gravity measurement.     

N形缝光线引入器太阳敏感器技术研究

为适应微小卫星发展的需求,提出了基于线阵电荷耦合器(Charge Coupled Devices, CCD)的N字形狭缝数字太阳敏感器研究方案,以减小系统功耗并降低系统复杂度。该方案通过采用带有N字形狭缝的光线引入器以及单个线阵CCD作为光线探测器,实现了太阳敏感器对两轴太阳角的精确计算。提出利用迭代算法和修正系数对系统折射误差进行修正的方法,进一步结合质心算法,能够快速准确修正系统误差,提高系统精度和分辨率。N型数字太阳敏感器视场角可达(±60°)×(±60°),在整个视场范围内定姿精度优于0.1°,功耗 300mW。该数字太阳敏感器具有低功耗、大视场角和高精度的特点,设计、算法均大大简化,实现了太阳敏感器的微型化,在各种微小卫星上有广阔的应用前景。     

嫦娥二号探测器轨道确定与支持

针对嫦娥二号探测器直接进入地月转移轨道、距月面100km高度捕获月球、完成既定任务后飞往日地第二拉格朗日平动点等飞行轨道方面的新特点,分析了定轨预报策略,利用事后精密轨道,全面评估了关键变轨点定轨预报和变轨后快速定轨的精度,其中,近月制动前3h定轨预报至近月点的位置误差为1km,速度误差为 0.3m/s 。利用不同月球引力场模型进行环月轨道精密定轨,根据实测数据残差分析和精密星历比对的结果,采用SGM100h引力场模型的定轨残差均方根最大。此外,针对嫦娥二号扩展任务,分析了不同测轨条件下的定轨精度,测量数据残差分析结果表明,在扩展任务中途修正前的定轨弧段内,测距、时延和时延率数据的残差分别为5m,5ns和1ps/s。     

基于ANSYS对遥感器铝合金镜头低温环境试验技术的研究

为了给新型遥感器用铝合金镜头提供良好的模拟试验环境,针对较低的温度以及较高的温度均匀性要求,为提高试验可靠性和工作效率,采用仿真计算与试验相结合的方式。运用ANSYS软件详细分析试验过程中的三维温度场,预测整个过程的降温趋势,以提前发现试验中可能存在的潜在问题并做出有效的改进。同时开展低温条件下的试验验证。结果表明:仿真计算值与试验结果趋势相符。通过仿真分析提前预测潜在的问题并对试验方案做出改进,有助于提高试验的可靠性和效率,也为日后的各类金属镜头的低温试验奠定了基础、积累了经验。