中国上空过渡流区大气月平均状态的模拟结果

利用美国海军研究实验室在MSIS系列模型基础上发展的大气模型NRLMSISE-00, 模拟研究了2001年—2013年中国上空过渡流区80～140 km高度的大气状态。对于中国东部和中部过渡流区, 基于模拟数据得到的月平均结果显示大气密度和温度呈现一致的变化趋势, 还表现出与太阳活动的显著关联。谱分析的结果显示, 在90 km高度以上大气密度呈现半年周期变化, 在90～110 km高度范围这种半年变化的幅度随纬度增大。在100 km高度, 上半年出现的半年周期过程中密度的最大、最小值分别出现在3月和6月, 明显超前中、高热层的半年周期过程。     

嫦娥三号“玉兔号”巡视器行为规划方法

为支持"玉兔号"巡视器完成对月面较大空间范围的科学探测,对动态任务进行快速规划,提出了一种基于人工智能领域智能规划技术的自动化任务规划方法。提出了行为持续时间和行为效果动态确定的时态规划模型(TP~(DDDE)),设计了描述TP~(DDDE)问题的规划领域定义语言PDDL——PDDL~(DDDE),以及针对TP~(DDDE)问题的启发式规划算法,运用Landmark知识分析规划问题结构,从而设计了合理反映动作前提评估顺序的启发函数。在嫦娥三号任务中,本文方法支撑"玉兔号"巡视器圆满完成了预期的科学探测任务。     

在强地磁活动期间热层大气成份和密度的变化

选用了１９７４－０７－０６,１９８２－０３－０２和１９８２－０９－０６三次强地磁活动时的Ａｐ值,由ＡＥ－Ｃ和ＤＥ－Ｂ卫星所测得的热层成份数据,进行统计分析,结果表明;在强地磁活动期间,热层大气密度涨落变化十分清晰、涨幅随高度增高而增大,高度６００ｋｍ附近涨幅可直达４倍,热层大气成份中Ｎ２的数密度涨幅最大,而原子氧的丰度在强地磁活动期间明显地下降。     

航天服关节力矩的数学模型

航天服关节力矩特性的数学表述是预测航天员出舱(EVA)作业强度、评估航天员疲劳度、规划EVA活动路径的重要基础。首先,分析了关节力矩的特性,提出建立数学模型的要求,阐述了Jiles-Atherton磁滞模型原理,以及磁滞模型与关节力矩特性的相合性。其次,利用模拟退火算法的思想对遗传算法进行了改进,并基于MATLAB软件实现。最终,对EVA航天服腕关节和肩关节力矩进行仿真,得到关节力矩在特定活动角度下的数学模型。仿真结果表明,针对关节力矩迟滞特性所得的关节力矩数学模型,能够更准确地描述关节活动力矩特性,计算所得模型可以更便捷地用于航天服工效学等相关研究领域。     

空间碎片自然衰减和太阳活动

分析研究了空间碎片数随太阳辐射流量Ｆ１０．７的变化;给出预报Ｆ１０．７长期变化的计算方法和预测空间碎片数的数学模型。结果显示：①强太阳活动造成空间碎片年增长率下降;②空间碎片数与太阳活动１１年变化密切相关,相关数为０．９;③空间碎片增长率约为发射率的两倍;④若发射率保持不变,则到２０２０年,大于１０ｃｍ的碎片数将达到１４５００;⑤若小碎片的增长为大碎片增长的两倍,则到２０２０年,大于１ｃｍ的碎片数可达１２５０００。     

航天员出舱活动地面试验综合复压系统控制技术

为了验证人-舱-服系统的可靠性和安全性,必须在地面做充分的模拟试验。地面试验综合复压系统为航天员的生命安全提供了可靠的试验环境。其中,测控系统采用的PCS7过程控制系统对关键环节均实现了热备冗余,满足试验过程控制要求,可靠地实现了综合复压系统的正常工作和紧急复压自动控制流程,并圆满地完成了人-舱-服联合试验。     

CHANGES OF THE THERMOSPHERE DENSITY IN THE SUNSHINE AND SHADE AREA OBSERVED BY "SZ-2" ATMOSPHERIC DENSITY DETECTOR

In this paper, thermosphere density data of "SZ-2" Atmospheric Density Detec tor From February to April 2001 are used to study the changes of the thermo sphere density in the sunshine and shaded area during solar and geomagnetic activity. The results show that in the sunshine area, the peak value of atmo spheric density changes as F10.7 varies; during geomagnetic activity, the peak value of atmospheric density in the shaded area increases as Ap increases, and start off with higher latitude, therefore move to lower latitude.     

神舟4号大气成分探测的新结果

神舟4号(SZ-4)大气成分探测器搭载在SZ-4留轨舱上于2002年12月30日发射入轨，在在轨运行的前3个多月中，正值地球南半球处于夏半球季节，并发生了多次中低强度的地磁扰动事件，SZ-4大气成分探测器测得了轨道舱运行高度上(330-362km附近)大气成分的响应变化和异常现象新结果．探测数据表明，中低强度的地磁扰动事件也能引起热层大气中主要成分O和N2的数密度值增高的响应变化．同样在进入地磁扰动峰期后较高纬度处出现了N2的异常增变和O的异常降变以及大气密度异常扰动的现象，但此期间所出现异常现象的地域与SZ-3和SZ-2大气成分探测器探测结果相反，它仅位于南半球较高纬度地区．     

A summary of the applications of a weighted average method determining times of solar cycle extrema

This paper is a summary of our recent researches on the applications of a weighted average method determining times of solar cycle extrema in the prediction of solar activity. Some correlation coefficients among the parameters in solar cycle according to this definition are higher than those according to the conventional definition. The descending time is found to be correlated (r = −0.77) with the ascending time 3 cycles earlier. The amplitude of solar cycle is found to be correlated (r = −0.77) with the max–max solar cycle length 2 cycles earlier. The ascending time is found to be correlated (r = −0.72) with the amplitude. A newly defined parameter called effective duration is found to be well correlated (r = 0.86) with the amplitude 5 cycles later. These correlations suggest that earlier cycles should influence later ones. The next (24th) solar cycle is estimated to start in March 2007 ± 7 months, reach its maximum in January 2011 ± 14 months, with a size of 150 ± 22, larger than those from some correlations according to the conventional definition.     

Kuafu and the studies of CME initiation

We first briefly review the current trend in the studies of coronal mass ejections (CMEs), then summarize some recent efforts in understanding the CME initiation. Emphasis has been put on the studies of Earth-directed CMEs whose associated surface activity and large scale magnetic source have been well identified. The data analysis by combining the MDI full disc magnetograms, vector magnetograms of active regions, EUV waves and dimmings, non-thermal radio sources, and the SOHO LASCO observations has shed new light in understanding the CME magnetism. However, the current studies seem to invoke new observations in a few aspects: (1) The observations which enable us to trace CMEs from the earliest associated surface activity to its initial acceleration and key development in the low corona in the height of 1–3 R; (2) The imaging spectroscopic observations which can be used to diagnose the early plasma outflow and the line-of-sight velocity in understanding the kinematics of CMEs; (3) The accurate timing from primary magnetic energy release, manifested by chromospheric activity, non-thermal radio bursts, and EUV, X-ray and γ-ray emissions, to the CME initiation, early acceleration and propagation, and the consequences in the interplanetary space and magnetosphere. The Kuafu Mission will meet the basic requirement for the new observations in CME initiation studies and serve as a monitor of space weather of the Sun–Earth system.