基于GPS散射信号的机载海面风场反演系统

提出了利用GPS散射信号构成机载海面风场反演系统,详细介绍了基于GPS散射信号的风场反演模型与散射信号相关功率的计算方法,给出了不同海面粗糙度下散射信号的相关功率曲线。分析了延迟映射接收机的工作模式,给出了某次飞行试验的数据分析结果。试验结果表明,文中所设计的延迟映射接收机能够准确地接收到GPS卫星信号的海面反射信号,并给出与理论分析一致的结论。     

A simulation of Martian gravity field recovery by using a near equatorial orbiter

An improvement to the Martian gravity field may be achieved by means of future orbiting spacecraft with small eccentricity and low altitude exemplified through a newly proposed mission design that may be tested in upcoming reconnaissance of Mars. Here, the near equatorial orbital character (with an inclination approximating 10°, eccentricity as 0.01 and semi-major axis as 4000 km) is considered, and its contribution to Martian gravity field solution is analyzed by comparing it with a hypothetical polar circular orbiter. The solution models are evaluated in terms of the following viewpoints: power spectra of gravity field coefficients, correlations of low degree zonal coefficients, precise orbit determination, and error distribution of both Mars free air gravity anomaly and areoid. At the same time, the contributions of the near equatorial orbiters in low degree zonal coefficients time variations are also considered. The present results show that the near equatorial orbiter allows us to improve the accuracy of the Martian gravity field solution, decrease correlation of low degree zonal coefficients, retrieve much better time variable information of low degree zonal coefficients, improve precise orbit determination, and provide more accurate Mars free air gravity anomaly and areoid around the equatorial region.     

利用数字高程模型自动检测火星表面陨石坑

为了克服利用影像识别陨石坑的诸多限制因素,利用"火星全球勘探者"(MGS)火星激光高度计(MOLA)得到的火星三维DEM数据,转换获得地形曲率,然后利用设定阈值将曲率图转换为二值图像,结合图像分割floodin算法可以得到待检测陨石坑,最后利用Hough变换可以检测出陨石坑。其成功率达到73.4%,可以有效地从DEM中识别陨石坑。利用DEM识别陨石坑的方法可以识别更多新的陨石坑,为现存的陨石坑目录提供新的数据信息。     

中国海洋卫星技术成就与展望

利用卫星探测海洋已经成为国际海洋环境与生物资源探测的最有效手段。文章介绍了我国成功发射的海洋一号A星和B星的主要技术指标以及获得的重要应用成果,并展望了未来我国海洋卫星的后续发展。     

天基海洋监视体系方案设计与综合评价

为应对海上作战平台的威胁,有效防御和打击这类目标,设计了5种天基海洋监视体系方案,通过利用模糊理论量化和聚合评价指标,利用层次分析法确定各层指标权重,对其进行了综合评价和优劣排序。所采用的模糊综合评价方法能够比较有效地处理定性、定量指标的量化与聚合问题,评价结果能够合理区分各方案的优劣情况。     

反潜巡逻机布放包围浮标阵应召搜潜建模与仿真

依据经典的浮标应召搜潜方法,结合实际搜潜过程,以某型反潜巡逻机为背景,建立了反潜巡逻机布放圆形阵、方形阵和三角形阵搜潜航路规划的数学模型。对3种阵形的搜潜效能进行分析,仿真了初始距离、潜艇初始位置散布、潜艇经济航速和海洋环境噪声级对浮标阵搜潜效能的影响。仿真结果分析表明:相同条件下,方形阵的搜潜效能要略高于圆形阵和三角形阵的搜潜效能;3种包围阵的搜潜效能均随初始距离、初始位置散布、潜艇经济航速和海洋环境噪声级的增大而降低。     

The Solar Wind Interaction With the Martian Ionosphere/Atmosphere

The interaction of the solar wind with the Martian exosphere and ionosphere leads to significant loss of atmosphere from the planet. Spacecraft data confirm that this is the case. However, the issue is how much is actually lost. Given that spacecraft coverage is sparse, simulation is one of the few ways for these estimates to be made. In this paper the evolution of our attempts to place bounds on this loss rate will be addressed. Using a hybrid particle code the loss rate with respect to solar EUV flux is addressed as well as a variety of numerical and chemical issues. The progress made has been of an evolutionary nature, with one approach tried and tested followed by another as the simulations are improved and better estimates are produced. The results to be reported suggest that the ion loss rates are high enough to explain the loss of water from Mars during earlier solar epochs.     

Exploring links between crater floor mineralogy and layered lunar crust

Floors of similar sized craters, representing material from similar depth horizons, have been studied to explore their suitability as mineralogy indicators at various depths within the lunar crust. Clementine UV–vis multispectral data was used to generate mineral abundance maps of crater floors and surroundings using a modified version of algorithm given by Pieters et al. (2001) [Pieters, C.M., Head, J.W., Gaddis, L., Jolliff, B. and Duke, M. Rock types of the south pole aitken basin and extent of basaltic volcanism, JGR (106) E11, 28001–28022, 2001.]. Substantial processing of the crater floor material due to variety of geological processes is evident in the generated maps, making straight forward interpretations difficult. However, systematic compositional trends in fresh craters on the floors of target craters seem to indicate the feasibility of such an effort.     

The first new application of the Mathematical Theory of Stochastic Processes to lunar and planetary science: Topography-Profile Diagrams of Mars

The Mathematical Statistics Theory (MST) and the Mathematical Theory of Stochastic Processes (MTSP) are different branches of the more general Mathematical Probability Theory (MPT) that can be used to investigate physical processes through mathematics. Each model of a stochastic process, according to MTSP, can provide one or more interpretations in the MST domain. A large body of work on impact crater statistics according to MST exists, showing cumulative crater frequency (N km⁻²) as a function of age (years) for some particular crater diameter. However, this is only one possible representation in the MST domain of the bombardment of the planetary surface modeled as a stochastic process according to MTSP. The idea that other representations are possible in the MST domain of the same stochastic process from MTSP has been recently presented. The importance of the approach is that each such mathematical-based interpretation can provide a large amount of new information. Coupled with MOLA data, Topography-Profile Diagrams (TPD) are one of the many examples that can provide a large amount of new information regarding the history of Mars. TPD consists of: (1) Topography-Profile Curve (TPC), which is a representation of the planet’s topography, (2) Density-of-Craters Curve (DCC), which represents density of craters, (3) Filtered-DCC (FDCC), which represents DCC filtered by a low-pass filter, included with the purpose of reducing the noise, and (4) Level-of-Substance-Over-Time Curve (LSOTC), which represents interpretation of the influence on the distribution of craters shown by FDCC. TPC uniquely corresponds to the computation of TPD, whereas DCC depends on algorithms for computing the elevation of each crater according to the topography, center coordinates, and radius of impact crater, and FDCC relies on the architecture of the custom designed low-pass filter for filtering DCC. However, all variations of DCC and FDCC, which includes the various impact crater data sets, showed a correlation among the density of craters and elevation over 70–80% of the planet surface. Additionally, if we assume that the ocean primarily caused the noted correlation, LSOTC offers a mathematical approach for estimating topographic change of the ocean’s extent over time. Accordingly, TPD is the first new practical application of MTSP to lunar and planetary sciences, showing correlation of topography to a physical process.