火星土壤物理力学特性分析

火星土壤既是火星表面探测活动的主要探测对象,也是表面探测器设计中需考虑的重要因素之一。火壤的物理力学特性将直接影响着陆器着陆缓冲系统、火星车移动系统等的设计。此外,在着陆器和火星车等表面探测器的地面研制过程中,需要研制模拟火壤,形成模拟的火星表面环境,开展相关的着陆器着陆缓冲性能、火星车移动性能等验证试验。迄今为止,人类已经有多个探测器登陆火星,获取了大量的有关火壤的信息,也研制了多种模拟火壤。通过对已有火壤和模拟火壤的物理力学特性分析,梳理出火壤物理力学特性的参数范围,可为我国火星探测器的研制提供参考。     

火星表面高氯酸盐生物转化及原位制氧工艺技术

火星表面极端缺氧条件及广泛分布的高氯酸盐所形成的强氧化环境,对人类登陆探测及后续宜居环境建设构成直接威胁.根据对火星表面高氯酸盐分布的探测成果,地球上高氯酸盐生物降解研究进展,以及人类登陆火星对资源和环境的需求,提出了利用生物方法转化火星表面高氯酸盐进行原位制氧的设想与工艺,对其工艺过程、影响因素、关键技术与难点、行星保护与副产物资源化、后续火星环境改造等进行了前瞻性分析,有望在火星上同时实现高氯酸盐无害化处理与氧气原位制备,化害为益,为火星探测提供新思路与新方法.     

基于高斯伪谱法的火星表面上升燃耗最优轨迹设计

火星上升器的设计与其轨迹设计紧密相关,而现有方法大都将MAV(Mars Ascent Vehicle)的分级优化和轨迹优化解耦计算,其计算效率低且鲁棒性较差。提出了一种基于高斯伪谱法的两级MAV分级与轨迹耦合多阶段优化算法,它以MAV的发射总质量最小为目标函数,并考虑了MAV设计约束、MAV的质量模型约束、轨迹的路径约束和控制约束等限制条件。利用该方法可以同时求得发射总质量最小的两级MAV分级参数和一条燃耗最优的上升轨迹,解决了由于不合理的两级MAV分级设计导致的轨迹优化算法无法收敛的问题。数值仿真结果表明该方法具有较快的收敛速度,且对初值选取的敏感度较小、具有较强的鲁棒性。     

美国“火星勘测轨道器”拍到在火星南极着陆的凤凰号表面披霜的最新图片

从所拍摄的图片可以看到,凤凰号表面覆盖了一层霜。这些新图片是于2009年7月30日和8月22日拍摄的,于11月4日对外公布。     

用于火星表面生命信息探测的激光拉曼技术进展

生命信息探测一直是深空探测中重要的一个部分。简要介绍了拉曼光谱技术探测有机物的优势和火星生命信息探测进展,以及常见的火星生命信息探测技术;重点概述了国内外用于火星有机物和生命信息探测的激光拉曼光谱技术的进展,分析总结了火星表面有机物质探测技术的发展趋势;最后简要概述了拉曼光谱技术在火星探测领域的发展前景。     

密集烘烤过程中烤房叶间风速指标的灰色关联聚类分析

在烘烤过程中,密集烤房内部不同位点的风速之间密切又复杂.为确定风速指标间的关系,测定了密集烤房内405个风速值,对15个风速指标进行了灰色关联聚类分析.结果表明：当聚类临界值为0.8时,15个风速指标可被聚为2类;当聚类临界值为0.7时,15个风速指标可被聚为1类.通过分析,密集烤房内部同一平面不同位点的风速差异较小,可视为均匀一致,密集烤房能够保证装烟室同一层烟叶整体上均处于同样的变色和干燥环境下,从而能够在理论上保证其烟叶相同的烘烤质量.     

美国2020火星车着陆区遴选进展及对2020中国火星任务着陆探测部分的一些思考

总结了近20年来火星探测的重要发现以及生命、气候和地质3个方面尚未解决的关键科学问题;介绍了美国国家航空航天局(NASA)2020火星探测任务的科学目标、科学载荷和着陆区选择的工程条件限制,并重点分析了经过3次着陆区选择研讨会,上百位行星科学家投票选取的排名前3的预选着陆区的地质情况。在此基础上,提出了对我国2020年火星任务的着陆探测部分的一些思考,并根据不同的任务目标(聚焦生命、气候和地质问题;支持载人火星探测的资源勘察;工程技术验证)提出了3个候选着陆区。     

空间物理过程时空协同探测的覆盖分析方法研究

针对空间物理过程时空协同探测任务的定量化探测覆盖分析需求, 在采用时空相关函数方法描述和分析空间物理时空过程的基础上, 提出一种基于θ-t_R覆盖图的探测覆盖分析方法. 通过分析不同设计方案在一定累计时间周期内的θ-t_R覆盖图, 根据其覆盖范围的不同选择所需要的设计方案. 采用该方法对两条共轨道面椭圆轨道的时空协同探测过程进行了定量的覆盖分析, 验证了该方法的有效性.     

Numerical simulations of the regional characteristics of dust transport on Mars

Using a Martian general circulation model (GCM), regions favorable for expansion of dust storms on Mars are identified. Dust transport simulations for the northern fall provide global maps of dust expansibility. These global maps show that dust injected from certain areas in the northern mid-latitudes tends to spread widely within a few days. The high expansibility of dust in such areas results from thermal tides, baroclinic waves, and quasi-stationary disturbances. Dust injected into the vast regions around Tharsis and the Sirenum–Aonia regions also tends to spread extensively. However, dust expansion around these two regions largely depends on the local time of dust injection. On the other hand, dust injected at high latitudes in either hemisphere does not spread extensively. Such global maps indicating regions favorable for dust storm expansion are a clue to understanding the expansion processes and climatology of great dust storms on Mars.     

太阳风对流效应对CME渡越时间的影响

基于Gopalswamy预报日冕物质抛射（CME）渡越时间的经验模型,选取1996-2007年间52个与地磁效应Dst<-50nT相关的CME事件以及10个引起特大磁暴（Dst<-200nT）的CME事件,结合ACE卫星在1AU处的太阳风观测资料,分析背景太阳风对流效应对CME到达1AU处渡越时间预报的影响.对于52个CME事件,考虑太阳风对流效应的影响后,预报的标准偏差由16.5h降为11.4h,修正后的误差分布趋向于高斯分布,并且68%事件的预报误差小于15h.对于10个引起特大磁暴的CME事件,考虑太阳风对流效应的影响后,预报的标准偏差由10.6h降低到6.5h,其中6个事件的预报误差小于5h.研究结果表明,对于CME事件,考虑背景太阳风对流效应的影响可以降低预报CME渡越时间的标准偏差,说明太阳风对流效应对预报CME事件渡越时间具有重要作用.     

Development of a micro-balance system for dust and water vapour detection in the Mars atmosphere

Quartz crystal piezoelectric sensors are suitable for deposition analyses that need very high sensitivity. Due to the wide working ranges and high performances, micro-balances can measure the mass settling in average Mars conditions during a period of months before saturation is reached. This ensures a proper use for short and long term water and dust deposition monitoring. Micro-balances have been studied, calibrated and used for the GIADA (grain impact analyser and dust accumulator) experiment for the ESA-Rosetta space mission. Experience on micro-balance performance study by dust deposition has been acquired and water vapour deposition studies are in progress in a Martian atmosphere simulation chamber. Preliminary results show that micro-balances are capable to detect up to partial pressure values corresponding to parts per billion of the typical Martian atmosphere.     

Automatic detection of typical dust devils from Mars landscape images

This paper presents an improved algorithm for automatic detection of Martian dust devils that successfully extracts tiny bright dust devils and obscured large dust devils from two subtracted landscape images. These dust devils are frequently observed using visible cameras onboard landers or rovers. Nevertheless, previous research on automated detection of dust devils has not focused on these common types of dust devils, but on dust devils that appear on images to be irregularly bright and large. In this study, we detect these common dust devils automatically using two kinds of parameter sets for thresholding when binarizing subtracted images. We automatically extract dust devils from 266 images taken by the Spirit rover to evaluate our algorithm. Taking dust devils detected by visual inspection to be ground truth, the precision, recall and F-measure values are 0.77, 0.86, and 0.81, respectively.     

Schumann resonance frequency and conductivity in the nighttime ionosphere of Mars: A source for lightning

We have solved the Maxwellian equations of electromagnetic waves which oscillate within the cavity formed in the lower ionosphere of Mars between 0 and 70?km. The electrical conductivity and Schumann Resonance (SR) frequencies are calculated in the lower ionosphere of Mars, in the presence of a major dust storm that occurred in Martian Year (MY) 25 at low latitude region (25°–35°S). It is found that the atmospheric conductivity reduced by one to two orders of magnitude in the presence of a dust storm. It represents a small dust layer at about 25–30?km altitudes where lightning can occur. We also found that the SR frequencies peak at?～18?km with values 19.9, 34.5 and 48.8?Hz for the modes l?=?1, 2 and 3, respectively, in the non-homogeneous medium. Our results indicate that practical or measurable values of SR are dependent on the altitudes.     

Observation of aphelion cloud belt over Martian tropics,its evolution,and associated dust distribution from MCS data

The present study uses five Martian years of observations from Mars Climate Sounder onboard Mars Reconnaissance Orbiter for investigating the Aphelion Cloud Belt (ACB) over the tropics. Analysis of zonal mean water ice column opacity suggests that the spatial extension of the ACB is mainly confined over the tropics and mid-latitudes (-20 – 40°N) during L_S ~ 45 – 135° (L_S = 0° signifies northern spring equinox). The ACB is seen primarily in the nighttime only due to the truncation of the daytime profile observations at significantly higher altitudes (at ~30 km). Zonal mean ice extinction profiles show ACB’s altitudinal range within ~10 – 40 km, and the existence of a thin cloud band in the absence of a thick ACB during aphelion season. Three phases of the ACB could be identified as the formation phase during L_S = 45 – 75° (phase 1), the peak phase during L_S = 76 – 105° (phase 2), and the decaying phase during L_S = 106 – 135° (phase 3). Observation of the cloud latitude belt shows a northward movement starting from phase 2, prominent over regions nearby Lunae Planum and Xanthe Terra. During this phase, the top level of thick clouds within the ACB decreases to ~20 km in the southern hemisphere, while it increases a little over the northern hemisphere (NH). The decreasing tendency continues in phase 3 over the entire region ?10 – 10°N, and the thick cloud base moves higher over the NH, though the vertical depth of it becomes narrower than phase 2. Temperature profiles do not show any noticeable influence on the northward evolution of the ACB. However, the study at a regional level indicates a possible association of upper tropospheric dustiness with the ACB’s evolution. The mechanism is evident in the correlation analysis mostly at an altitude range of ~18 – 35 km. The migrating semidiurnal tide (SMD) as a proxy of dust or water ice forcing, and the calculated upper tropospheric dust radiative heating, shows an apparent northward movement of their peak amplitude within the three phases of the ACB. This match between the spatiotemporal variations of the SMD and the water ice was not observed previously. However, the correlating behavior seems to be prominent in the areas nearby Lunae Planum and Xanthe Terra and the upper-tropospheric region of the atmosphere.     

中纬度地磁暴期间热层垂直风响应机制的模拟

基于TIMEGCM模型,研究了2005年9月10日中纬度地磁暴期间热层（100~650 km）水平风场变化对垂直风的影响。通过连续性方程诊断分析了暴时引起垂直风场变化的机制,结果表明：250 km以上的垂直风场取决于水平风场的变化,而250 km以下的垂直风场由较高高度的垂直风拉动;在地磁暴初相开始时,经向风场相比纬向风场对暴时250 km以上的垂直风场影响更为显著,随着地磁扰动增强,纬向风场对垂直风场变化的贡献更大;温度场对地磁暴的响应遵循同样规律,扰动开始时,温度沿经线传播更快,经向风变化更大,扰动增强后,温度沿纬线传播更快,纬向风变化更大。