Coma morphology and dust emission pattern of comet Halley

This contribution starts with a short overview on cometary dust modelling and then focuses on the application of coma modelling with respect to in-situ measurements of cometary dust and ground based observations. The fountain model, valid for the dynamics of small cometary dust particles, is discussed. Models using Keplarian theory for the motion of the dust particles are outlined and the ESOC coma model is presented. Some direct applications of this model to analyse the results of the recent spacecraft flybys of comet Halley, as dust flux profiles, particle ground tracks and envelope positions, are shown. To compare the model with ground-based astronomical observations, the utilization of the ESOC coma model for the generation of synthetic images is demonstrated and some future prospects of this technique are outlined.     

无人机定向天线自跟踪系统研究

为了满足无人机(UAV)远距离通信的需要,设计研制了以无人机位置信息为引导的地面定向天线自跟踪系统。基于实时获取定向天线载车位置、速度、方位和俯仰角等信息,实现了定向天线在运动中对目标进行自动跟踪的能力,提高了系统的机动性和隐蔽性。针对目前利用2点位置来计算目标角的方法存在需要通过相对位置才能确定实际目标角的不足,提出了一种不需要考虑2点相对位置就能直接计算出目标角的计算方法,为工程应用带来了方便。针对定向天线地面载车在机动时GPS信号容易受干扰,从而造成跟踪目标丢失,以及因无人机位置信息更新频率较低而造成的跟踪系统运动抖动、跟踪误差较大等问题,提出了一种基于速度对位置进行预测平滑的控制策略,有效解决了以上问题,并显著提高了跟踪精度。设计研制了定向天线自跟踪系统的软硬件,并进行了测试,结果表明:研制的定向天线具有机动跟踪能力和较高的跟踪精度,能满足无人机对定向天线自跟踪的需要。      

双麦克斯韦分布下极区中层尘埃粒子带电研究

在大功率微波照射下，极区中层夏季回波（PMSE）会立刻消失，该现象被称为极区中层加热现象.在大功率微波照射极区中层时，电子在微波电场加速下产生的定向运动速度与热运动速度可以比拟，极区中层的尘埃等离子体服从双麦克斯韦分布.基于双麦克斯韦分布下尘埃粒子充电理论给出极区中层尘埃粒子的电荷分布，比较了大功率微波对极区中层加热前和加热时，尘埃粒子电荷以及极区中层电子浓度的变化.结果表明，采用大功率微波装置加热极区中层会影响电子对尘埃粒子的充电进而导致电子浓度变化，这对解释极区中层加热现象具有重要意义.      

Cosmic dust measurements in lunar orbit

On 15th February 1992, ISAS space engineering satellite HITEN was successfully inserted into an elliptical orbit around the moon with perilune between some 100 km and 8000 km and apolune of about 50.000 km. On board was a small scientific experiment designed to detect cosmic dust particles, MDC - Munich Dust Counter. During a period of more than one year, until Hiten's hard landing on the moon surface at 10th of April 1993 (UTC), measurements of impact velocity, mass and crude flight direction of micrometeoroid particles have been performed. In total 150 cosmic dust impacts were detected and evaluated. From these measurements, the impact rate versus time and the dust flux versus distance from the moon are derived. The evidence of moon ejecta and some indications of particles which are orbiting the moon will be discussed. The spatial distribution of the measured particles is shown in lunarcentric as well as in heliocentric coordinate systems. The directional distribution is also given, showing the different populations of cosmic dust particles. Finally, the gathered data will be compared with previous results from measurements in the vicinity of the Earth and in the geomagnetic tail region.     

Developing a dust storm detection method combining Support Vector Machine and satellite data in typical dust regions of Asia

Enhancing the dust storm detection is a key part for the environmental protection, human healthy and economic development. The goal of this paper is to propose a new Support Vector Machine (SVM)-based method to automatically detect dust storms using remote sensing data. Existing methods dealing with this problem are usually threshold-based that are of great complexity and uncertainty. In this paper we propose a simple and reliable method combining SVM with MODIS L1 data and explore the optimal band combinations used as the feature vectors of SVM. The developed method was evaluated by MODIS and OMI data qualitatively and quantitatively on three study sites located in the Arabian Desert, Gobi Desert and Taklimakan Desert, and it was also compared to three other traditional methods based on their accuracy, complexity, reliability and sensitivity to thresholds. The detection results demonstrated that the combination of (Band7 − Band3)/(Band7 + Band3) ((B7 − B3)/(B7 + B3)), Band20 − Band31 (B20 − B31), and Band31/Band32 (B31/B32) can detect the dust storms more precisely than other individual bands or their combination. The comparison among those cases indicated that the proposed automatic method exhibited an advantage of minimizing the uncertainty and complexity, which were the limits of defining thresholds based on the threshold-based methods. The conclusions can provide references for studies that focus on statistical-based dust storm detection.     

The interplanetary dust environment beyond 1 AU and in the vicinity of the ringed planets (tutorial talk)

The dust population at 1 AU is known for all sizes between μm and cm to an accuracy better than one order of magnitude. It was observed by Helios that the fine grained dust (μm to 100 μm) decreases with increasing sun distance ∞ r^?1.3, at least between 0.3 and 1 AU /1/.Two Pioneer $\text{10}\text{11}$ dust experiments observed the dust distribution beyond 1 AU in the 10 to 100 μm diameter size range for the first time directly with contradicting results. The penetration experiment saw a constant flux out to 20 AU while the optical experiment observed a decrease of the dust number densities until 3.3 AU, but no scattered light was recorded further out. An attempt is made to explain these observations on the basis of the socalled ‘Greenberg’-particles: cometary core/mantle grains with organic mantle material. The observed enhancement of the dust flux by 1 or 2 orders of magnitudes near Jupiter and Saturn are interpreted as being caused by gravitational focussing, ejecta from jovian/saturnian satellites and electrostatic fragmentation products.     

月尘环境效应及地面模拟技术

介绍了月球尘的特点及其对探月活动的影响。在分析月球尘环境及其对月面探测器污染、磨损、阻塞、静电效应的基础上,对月球尘环境模拟技术、月球尘扬尘及其运动学和动力学规律、月球尘效应防护及试验评价方法等研究方向和重点提出了一些初步看法。针对研究内容的需求,梳理出一台完整的月球尘地面模拟试验设备应具备真空、温度、太阳风、太阳紫外、月球尘、月面电场、月面磁场等环境因素。在此基础上,设计了一种月球尘地面模拟试验装置方案,并对月球尘环境效应试验方法进行了初步讨论。为月球探测后期任务条件保障建设及相关研究工作提供参考。     

火星沙尘环境光学图像增强方法

针对火星探测器着陆时沙尘天气对机器视觉的影响,提出一种去除沙尘天气对光学成像影响的方法,为视觉系统提供清晰输入图像。首先对受沙尘天气影响的图像建立模型,然后求取模型中大气光值与透射系数值。对于大气光值的计算采用基于四叉树细分的方法,在最小值图像上搜寻指定阈值面积中灰度均值最大的区域,在初始图像中相同区域计算各通道均值,作为大气光值。在此基础上计算透射系数,完成清晰图像的恢复。通过对受沙尘影响图像测试表明,该方法能够将受沙尘影响的图像恢复成清晰的图像。即使在复杂的环境中,该方法对光照变化、沙尘强度变化和场景变化等仍具有较好的效果。与其他方法相比,本文方法在去除沙尘对光学图像影响方面效果较好,在恢复图像评价指标等方面优于其他方法,能够进一步提高图像清晰度,为光学图像的后期处理提供更丰富信息。      

基于双轴旋转的惯导系统误差自补偿技术

针对陀螺漂移影响惯导系统长时间导航精度的问题,提出了一种基于双单元体结构的误差自补偿方案.通过单元体的连续正反旋转,可以实现对所有方向上陀螺常值漂移的调制,从而大幅提高惯导系统的精度.对常值漂移、刻度系数误差、安装误差和角度随机游走等主要误差源的误差特性进行了分析,同时讨论了旋转机构精度对系统调制性能的影响.利用自行研制的双轴旋转调制式激光捷联惯导系统进行了多次海上试验,试验结果表明该方案可行,在不改变惯性器件精度的前提下,可提高系统精度一个量级以上.     

Star angle/ double-differenced pulse time of arrival integrated navigation method for Jupiter exploration

Pulsar navigation is a promising autonomous navigation system for spacecraft, which is applicable to the entire solar system. However, the pulsar’s directional error and the onboard clock error are two types of systematic errors that seriously reduce navigation accuracy. To solve this problem, a star angle/double-differenced pulse time of arrival(SA/DDTOA) integrated navigation method is proposed. Since measurements obtained by observing different pulsars contain the same clock errors, the measurements can be differed to eliminate the common clock error. Then, the pulsar-differenced measurements at neighbor filtering time can be differed to suppress the effect of the pulsar’s directional error on navigation precision. Star angle is used to obtain absolute navigation information, which denotes the angles between the light of sight of Jupiter and that of its background stars. Simulation results demonstrate that the proposed method can eliminate the influence of the onboard clock error and greatly weaken the effects of the pulsar’s directional error. The navigation accuracy is better than the traditional star angle/pulse time of arrival integrated navigation method and star angle/pulse time difference of arrival integrated navigation method. In addition, the navigation accuracy of the SA/DDTOA integrated navigation method is less affected by Jupiter’s ephemeris error. This work greatly reduces the influence of common systematic errors in pulsar navigation on navigation accuracy.     

Effects of lunar and mars dust simulants on HaCaT keratinocytes and CHO-K1 fibroblasts

Exposure to lunar dust during Apollo missions resulted in occasional reports of ocular, respiratory and dermal irritations which showed that lunar dust has a risk potential for human health. This is caused by its high reactivity as well as its small size, leading to a wide distribution also inside habitats. Hence, detailed information regarding effects of extraterrestrial lunar dusts on human health is required to best support future missions to moon, mars or other destinations. In this study, we used several methods to assess the specific effects of extraterrestrial dusts onto mammalian skin by exposing HaCaT keratinocytes and CHO-K1 fibroblasts to dusts simulating lunar or mars soils. These particular cell types were chosen because the skin protects the human body from potentially harmful substances and because a well orchestrated program ensures proper wound healing. Keratinocytes and fibroblasts were exposed to the dusts for different durations of time and their effects on morphology and viability of the cells were determined. Cytotoxicity was measured using the MTT assay and by monitoring culture impedance, while phalloidin staining of the actin cytoskeleton was performed to address structural integrity of the cells which was also investigated by propidium iodide intake. It was found that the effects of the two types of dust simulants on the different features of both cell lines varied to a considerable extent. Moreover, proliferation of HaCaT keratinocytes, as analyzed by Ki67 labeling, was suppressed in sub-confluent cultures exposed to lunar dust simulant. Furthermore, experimental evidence is provided for a delay in regeneration of keratinocyte monolayers from scratch-wounding when exposed to lunar dust simulant. The obtained results will facilitate further investigations of dust exposure during wound healing and will ease risk assessment studies e.g., for lunar lander approaches. The investigations will help to determine safety measures to be taken during extraterrestrial expeditions in order to minimize risks to human health associated with exposure of human skin to dust contaminants.     

直升机吊挂流场数值模拟与尾鳍设计分析

根据已知的直升机吊挂的几何尺寸,利用CAD软件建立了两种吊挂的三维模型.利用图像测绘的方法对第1种吊挂尾鳍进行了初步设计,通过计算流体力学(CFD,Computational Fluid Dynamics)方法对带尾鳍的吊挂模型进行了计算与分析,气动力计算结果与理论计算结果吻合较好.此外,对第2种UH-60黑鹰直升机带尾鳍吊挂进行了CFD计算,考察了尾鳍对吊挂流场的影响.通过对两种带尾鳍的直升机吊挂情况的计算分析,证明了尾鳍对保证吊挂在飞行过程中的航向稳定性具有关键的作用,进而提出了一种基于无空气阻尼力假设的直升机吊挂尾鳍尺寸的设计方法,并对第2种吊挂状态下的尾鳍尺寸进行了计算设计.计算所得到的尾鳍面积对航向稳定性的影响结果与国外风洞实验结果保持一致.     

悬浮月尘的遮挡模型

探月活动中,月表的尘埃会对太阳翼等光电器件的工作效率造成严重影响.基于附着月尘的遮挡模型,从立体空间的角度分析了悬浮月尘对工作器件的遮挡,提出了悬浮月尘的单粒度遮挡模型,利用月尘的平均粒度可计算在指定立体空间内,定量月尘造成的遮挡量;引入月尘的粒度分布函数,提出了悬浮月尘的多粒度遮挡模型,能够计算已知粒度分布函数的月尘在指定立体空间内造成的遮挡量;通过设计悬浮月尘遮挡的仿真实验,分别利用3种不同粒度大小的月尘进行实验,实验数据与悬浮月尘的单粒度、多粒度遮挡模型的理论计算值都较好吻合,实验结果证实了悬浮月尘遮挡模型的正确性与可靠性.      

The MAGO experiment for dust environment monitoring on the Martian surface

Among the main directions identified for future Martian exploration, the study of the properties of dust dispersed in the atmosphere, its cycle and the impact on climate are considered of primary relevance. Dust storms, dust devils and the dust “cycle” have been identified and studied by past remote and in situ experiments, but little quantitative information is available on these processes, so far. The airborne dust contributes to the determination of the dynamic and thermodynamic evolution of the atmosphere, including the large-scale circulation processes and its impact on the climate of Mars. Moreover, aeolian erosion, redistribution of dust on the surface and weathering processes are mostly known only qualitatively. In order to improve our knowledge of the airborne dust evolution and other atmospheric processes, it is mandatory to measure the amount, mass-size distribution and dynamical properties of solid particles in the Martian atmosphere as a function of time. In this context, there is clearly a need for the implementation of experiments dedicated to study directly atmospheric dust. The Martian atmospheric grain observer (MAGO) experiment is aimed at providing direct quantitative measurements of mass and size distributions of dust particles, a goal that has never been fully achieved so far. The instrument design combines three types of sensors to monitor in situ the dust mass flux (micro balance system, MBS) and single grain properties (grain detection system, GDS + impact sensor, IS). Technical solutions and science capabilities are discussed in this paper.     

Nonthermal effects on the cylindrical dusty ion shocks in nonthermal viscous space plasma

The propagating cylindrical shock dust ion wave (CDISW) in dusty four component plasma with three viscous component (ion and two polarity charged grains) has been introduced. The three dimensional (3D) Cylindrical Burgers (CB) equation is derived. The propagating cylindrical shock characteristics are established to becomes a very significantly improved by the supports of electron nonthermality, ion and negative (positive) kinematics viscosity coefficients. Furthermore, the shock strength depends on cylindrical directions. The obtained results may be profitable in understanding both the laboratory and space applications of plasmas.     

近似函数用于材料腐蚀的数学建模

将近似函数引进到材料腐蚀的数学建模中,根据腐蚀数据特点,提出分段建模概念,并分别与灰色GM(1,1)模型、动态数据双向差分模型和幂函数模型对比.结果表明,这种近似函数模型的精度除普遍高于其它3种模型外,还具有很强的适用性,在工程上具有一定的应用前景.同时,由经验变换模型和该近似函数模型的数值处理推测认为,腐蚀过程中可能存在"腐蚀临界点".     

基于多特征融合的电磁换向阀故障模式识别

为提高基于驱动端电流检测的电磁换向阀故障诊断方法的可靠性和识别准确度，开展了电磁换向阀故障模式识别方法研究。提出一种基于多特征融合的方法对电流信号时频分析和时域参数的特征值提取融合；通过设计电磁换向阀驱动端电流信号的采集实验，获取电磁换向阀驱动端电流的时域信号和二阶变化率的多特征曲线，提取时域参数及二阶变化率相应频带能量作为特征值，构建多特征融合的特征向量；采用基于径向基核函数的多分类支持向量机对电磁换向阀进行模式识别。结果表明：基于多特征融合的支持向量机较基于能量特征值的支持向量机可提升8.7%的识别精度和42.11%的验证准确率。     

Improvement of the GRACE star camera data based on the revision of the combination method

The new release of the sensor and instrument data (Level-1B release 02) of the Gravity Recovery and Climate Experiment (GRACE) had a substantial impact on the improvement of the overall accuracy of the gravity field models. This has implied that improvements on the sensor data level can still significantly contribute to arriving closer to the GRACE baseline accuracy. The recent analysis of the GRACE star camera data (SCA1B RL02) revealed their unexpectedly higher noise. As the star camera (SCA) data are essential for the processing of the K-band ranging data and the accelerometer data, thorough investigation of the data set was needed. We fully reexamined the SCA data processing from Level-1A to Level-1B with focus on the combination method of the data delivered by the two SCA heads. In the first step, we produced and compared our own combined attitude solution by applying two different combination methods on the SCA Level-1A data. The first method introduces the information about the anisotropic accuracy of the star camera measurement in terms of a weighing matrix. This method was applied in the official processing as well. The alternative method merges only the well determined SCA boresight directions. This method was implemented on the GRACE SCA data for the first time. Both methods were expected to provide optimal solution characteristic by the full accuracy about all three axes, which was confirmed. In the second step, we analyzed the differences between the official SCA1B RL02 data generated by the Jet Propulsion Laboratory (JPL) and our solution. SCA1B RL02 contains systematically higher noise of about a factor 3–4. The data analysis revealed that the reason is the incorrect implementation of algorithms in the JPL processing routines. After correct implementation of the combination method, significant improvement within the whole spectrum was achieved. Based on these results, the official reprocessing of the SCA data is suggested, as the SCA attitude data are one of the key observations needed for the gravity field recovery.     

Sunyaev-Zel'dovich effect and the dust emission in the galaxy clusters

It is shown that if the dust is present in the hot intergalactic gas, the galaxy cluster must be very bright source of far infrared emission. This emission can be observed by modern IR astronomy methods. At the same time, taking realistic assumptions about the intergalactic dust nature, it is impossible to explain negative results of the attempts made at observational detecting the Sunyaev-Zel'dovich effect in the centimeter wavelength region as the compensation of the expected decrements by the dust grains emission.     

多星分布式无源相干定位方法

针对方向性辐射源信号主瓣波束窄测向定位精度不足的问题，提出多星分布式无源相干定位方法。首先，根据参考星接收到的主瓣强信号对辐射源位置进行粗定位，并根据粗定位信息对频移进行补偿；随后，将参考星信号分发至临近卫星，在粗定位范围内对相干星接收到的旁瓣弱信号进行互相关搜索，解算时差信息；然后，采用多星时差定位体制估计辐射源精确位置；最后对提出算法进行了Cramer-Rao下界分析，并通过仿真实验对算法进行验证。仿真结果表明，算法在弱信号信噪比(SNR在-40～0 dB)的情况下，定位误差能够快速逼近Cramer-Rao下界，并且能够有效提高辐射源的定位精度。