月球南极着陆区关键特性分析

与月球中低纬度着陆区不同,月球南极地区地形地貌条件较为恶劣,太阳高度角低,对地可见与不可见周期较长,这些关键特性都对南极着陆探测任务提出了挑战。文章结合国内外已开展的研究工作,对南极地区的光照条件、对地可见、地形地貌等方面进行了分析和总结,得到了上述关键特性的规律。南极地区不存在永久光照区,但存在一些几百米尺度的4~9个月的准连续光照区,着陆器的光照条件与着陆器高度密切关联;南极地区光照条件和对地可见受地形影响较大;在50m基线情况下,备选着陆区域平均坡度比较平缓(0°~5°);着陆器尺度5m基线情况下,不同备选着陆区域平均坡度相差较大,最大平均坡度可以达到25°。根据上述分析,对我国开展月球南极探测的任务规划和探测器系统设计提出了建议,主要包括着陆区的选择及探测器主要功能组成等。     

航天器仪表与照明分系统设计和发展

航天器仪表与照明分系统承担着飞行器与航天员信息交互的任务,为航天员在轨工作、生活提供支持。分系统功能包括信息显示提示、越限报警提示、手动操作、工作生活照明、休闲娱乐等。文章给出了航天器仪表与照明分系统设计思路及分系统设计组成;分析了分系统技术应用情况;对应航天器设计和应用结果,提出了后续航天器的技术发展思路和设想。     

太阳矢量在行星际探测器姿态估计中的应用研究

在基于矢量观测的行星际探测器姿态确定中,参考矢量的几何关系是影响姿态估计精度的一个重要因素。针对这一问题,本文提出了一种利用太阳矢量来提高探测器姿态估计精度的最优算法。该方法在引入太阳矢量的基础上,将星敏感器测得的姿态四元数转化为两个互相垂直的参考矢量,并根据敏感器的测量精度计算相应的规范化权值系数;结合姿态四元数估计算法,给出最小二乘意义下的探测器最优姿态估计。最后,以深度撞击任务的实际飞行数据对本文所提算法进行验证。仿真结果表明,引入太阳矢量后的三轴姿态角估计误差小于150μrad,完全满足深度撞击任务的要求。     

具有几何和光照不变性的不变矩构建研究

为了解决现有的光照变化条件下仿射不变矩识别不稳健的问题,提出了一种归一化光照仿射不变矩,即采用一种光照模型,基于Jan Flusser仿射不变矩,推导出一种归一化光照仿射不变矩,并且从理论上证明了该方法在各种仿射变换下的稳健性,然后通过对比实验验证了该方法在光照强度、方向和颜色改变下的不变性.实验结果表明,与当前主流的光照不变矩方法相比,该方法不仅适合灰度图像也适合彩色图像,在光照方向改变下,图像的倾斜运动中识别度提高了35％;在线性光照强度改变下,图像的倾斜运动中识别度提高了85％;在光照颜色改变下,图像的平移和旋转运动中识别度提高了7.8％;以多种卫星模型图像为实验对象,在光照改变下,彩色图像和灰度图像的识别度平均提高了36％以上,且计算简单,更适合于航天器目标的识别.     

一种相变热图的图像处理方法

相变热图技术中,为了得到风洞试验模型表面的热流分布,必须对相变热图序列进行相变线提取.首先通过特殊的时-空变换,将所有原始序列图像的直接分割转化为对少量合成图像的分割,在减小计算量的同时较好地解决了原始图像中由于相变区域模糊而难以分割的问题.同时,为了解决由于模型表面存在镜面反射造成的模型头部区域相变线提取不准确,引入镜面反射模型,并通过分割和参数求取过程的迭代执行计算出反射模型各参数,对合成图像进行整体性亮度补偿并最终得到良好的分割结果.最后根据提取出的相变线位置和材料相变温度,完成热流值的计算.通过比较表明本文结果更为准确合理,也验证了所提出分割方法的有效性,促进相变测温技术的广泛应用.     

Asymmetric precipitation in a coronal loop as explanation of a singular observed spectrum

Almost 10 years of solar submillimeter observations have shown new aspects of solar activity, such as the presence of rapid solar spikes associated with the launch of coronal mass ejections and an increasing submillimeter spectral component in flares. We analyse the singular microwave–submillimeter spectrum of an M class solar flare on 20 December, 2002. Flux density observations measured by Sun patrol telescopes and the Solar Submillimeter Telescope are used to build the radio spectrum, which is fitted using Ramaty’s code. At submillimeter frequencies the spectrum shows a component different from the microwave classical burst. The fitting is achieved proposing two homogeneous sources of emission. This theoretical fitting is in agreement with differential precipitation through a magnetically asymmetric loop or set of loops. From a coronal magnetic field model we infer an asymmetric magnetic structure at the flare location. The model proposed to quantify the differential precipitation rates due to the asymmetry results in a total precipitation ratio Q₂/Q₁≈10⁴–10⁵, where Q₁(Q₂) represents the total precipitation in the loop foot with the high (low) magnetic field intensity. This ratio agrees with the electron total number ratio of the two sources proposed to fit the radio spectrum.     

Driving major solar flares and eruptions: A review

This review focuses on the processes that energize and trigger M- and X-class solar flares and associated flux-rope destabilizations. Numerical modeling of specific solar regions is hampered by uncertain coronal-field reconstructions and by poorly understood magnetic reconnection; these limitations result in uncertain estimates of field topology, energy, and helicity. The primary advances in understanding field destabilizations therefore come from the combination of generic numerical experiments with interpretation of sets of observations. These suggest a critical role for the emergence of twisted flux ropes into pre-existing strong field for many, if not all, of the active regions that produce M- or X-class flares. The flux and internal twist of the emerging ropes appear to play as important a role in determining whether an eruption will develop predominantly as flare, confined eruption, or CME, as do the properties of the embedding field. Based on reviewed literature, I outline a scenario for major flares and eruptions that combines flux-rope emergence, mass draining, near-surface reconnection, and the interaction with the surrounding field. Whether deterministic forecasting is in principle possible remains to be seen: to date no reliable such forecasts can be made. Large-sample studies based on long-duration, comprehensive observations of active regions from their emergence through their flaring phase are needed to help us better understand these complex phenomena.     

Coronal fast wave trains of the decimetric type IV radio event observed during the decay phase of the June 6, 2000 flare

The 22 min long decimetric type IV radio event observed during the decay phase of the June 6, 2000 flare simultaneously by the Brazilian Solar Spectroscope (BSS) and the Ond?ejov radiospectrograph in frequency range 1200–4500 MHz has been analyzed. We have found that the characteristic periods of about 60 s belong to the long-period spectral component of the fast wave trains with a tadpole pattern in their wavelet power spectra. We have detected these trains in the whole frequency range 1200–4500 MHz. The behavior of individual wave trains at lower frequencies is different from that at higher frequencies. These individual wave trains have some common as well as different properties. In this paper, we focus on two examples of wave trains in a loop segment and the main statistical parameters in their wavelet power and global spectra are studied and discussed.