雷暴天气过程中降水结构与闪电活动特征个例研究

为深入分析四川雷暴天气过程中降水和闪电活动特征,运用统计与对比方法,对四川东南部一次雷暴过程中闪电活动及降水结构之间的特征进行研究。结果表明,强降水易发生在低层辐合,高层辐散的流场中,局部地区最大降水强度发生在2~5km高度。降水开始1h后,地闪频数达到最高,地闪主要以负地闪为主,正地闪不活跃。对闪电活动与亮温分布关系知,闪电活动主要发生在低于220K降水云内,闪电活动发生的区域与降水落区一致。对总闪与地闪的分布知,负地闪主要分布在总闪的外围。通过对四川雷暴过程的研究,对雷暴预报有一定的指导意义。     

IKONOS影像生产1∶10 000地理信息产品的研究

简要介绍了IKONOS卫星遥感影像适用于地理信息产品生产的特点,然后通过试验生产,并与传统的航片相比较,详细分析了利用IKONOS影像作为数据源生产1∶10000基础信息产品在精度、生产流程、工作效率、生产周期、外业工作量和价格等方面的情况。     

不同岩性火山岩力学性质实验研究

黄沙坨地区位于辽河断陷盆地东部凹陷中段,古近纪沙河街组第三段沉积时期发育了巨厚的火山岩,为该区形成火山岩油气藏奠定了成藏条件。由于油层岩石的力学性质,影响着油田生产,因此,经过实验室对不同岩性的火山岩力学性质的试验测试,得到油田生产所需的相关的力学参数及相关的地质信息,为油田勘探、开发及相关的工程设计发挥重要作用。试验结果表明,粗面岩以张性破裂为主,玄武岩以剪切破裂为主。这对油田研究水力压裂裂缝形态及储层天然裂缝形态提供了重要的地质依据。软化系数的较大波动,表现出地下流体对油层岩石的环境作用。     

石羊河下游人工梭梭林土壤呼吸变化特征及其与水热因子的关系

土壤呼吸不仅是反映土壤生物活性的重要指标,也是全球碳循环研究中备受关注的热点问题。在地处典型干旱区的石羊河下游,以流动沙丘和去除土壤结皮人工梭梭林为对照,采用LI-8100土壤碳通量监测系统研究了栽植约40 a、30 a、10 a和5 a的人工梭梭林生长季和非生长季的土壤呼吸日变化,并分析了土壤水分和温度对土壤呼吸的影响。结果表明：（1）不同林龄梭梭林生长季和非生长季土壤呼吸速率的日变化均为明显的单峰曲线,且呈现出一定的波动性,日最大排放速率出现在12:00～14:00时,最小值出现在8:00时左右。（2）梭梭林营造和去结皮处理显著提高了沙漠土壤呼吸速率,而且不同林龄土壤呼吸速率大体上随着种植年限的增加而递增,表现为MC >40 a>30 a>10 a>MS >5 a,非生长季表现为MC >40 a>10 a>5 a>30 a>MS。（3）不同林龄梭梭林土壤呼吸速率均具有明显的季节变化特征,生长季（8 月）的土壤呼吸作用明显强于非生长季（1月）。（4）相关性分析表明,生长季和非生长季土壤呼吸均与0～5 cm土壤水分显著相关,且均呈二次曲线关系,分别为Y =-0.205 8X ²+0.946 5X-0.316 6（R ² =0.506 ²,P= 0.041 7）和Y= 0.118 7 X ²+0.156 3X+0.118 8（R ²=0.675 7,P =0.001 1）;但与10 cm土壤温度的相关性不显著,土壤水分是影响人工梭梭林土壤呼吸的关键因素。该研究进一步证明了人工梭梭林的营造有效改善了沙漠土壤的生物活性,提高了土壤碳通量水平,以土壤结皮破坏为基本特征的人工梭梭林退化和沙漠化必然在短期内加剧碳排放。因此,需要在沙漠地区合理营造人工林,并在造林和林业管理过程中注意保护土壤结皮,以减少CO²排放。     

Research on Parallel Algorithms for uv-faceting Imaging

The uv-faceting imaging is one of the widely used large field of view imaging technologies, and will be adopted for the data processing of the low-frequency array in the first stage of the Square Kilometre Array (SKA1). Due to the scale of the raw data of SKA1 is unprecedentedly large, the efficiency of data processing directly using the original uv-faceting imaging will be very low. Therefore, a uv-faceting imaging algorithm based on the MPI (Message Passing Interface)+OpenMP (Open Multi-Processing) and a uv-faceting imaging algorithm based on the MPI+CUDA (Compute Unified Device Architecture) are proposed. The most time-consuming data reading and gridding in the algorithm are optimized in parallel. The verification results show that the results of the proposed two algorithms are basically consistent with that obtained by the current mainstream data processing software CASA (Common Astronomy Software Applications), which indicates that the proposed two algorithms are basically correct. Further analysis of the accuracy and total running time shows that the MPI+CUDA method is better than the MPI+OpenMP method in both the correctness rate and running speed. The performance test results show that the proposed algorithms are effective and have certain extensibility.     

Study of Star/Galaxy Classification Based on the XGBoost Algorithm

Machine learning has achieved great success in many areas today. The lifting algorithm has a strong ability to adapt to various scenarios with a high accuracy, and has played a great role in many fields. But in astronomy, the application of lifting algorithms is still rare. In response to the low classification accuracy of the dark star/galaxy source set in the Sloan Digital Sky Survey (SDSS), a new research result of machine learning, eXtreme Gradient Boosting (XGBoost), has been introduced. The complete photometric data set is obtained from the SDSS-DR7, and divided into a bright source set and a dark source set according to the star magnitude. Firstly, the ten-fold cross-validation method is used for the bright source set and the dark source set respectively, and the XGBoost algorithm is used to establish the star/galaxy classification model. Then, the grid search and other methods are used to adjust the XGBoost parameters. Finally, based on the galaxy classification accuracy and other indicators, the classification results are analyzed, by comparing with the models of function tree (FT), Adaptive boosting (Adaboost), Random Forest (RF), Gradient Boosting Decision Tree (GBDT), Stacked Denoising AutoEncoders (SDAE), and Deep Belief Nets (DBN). The experimental results show that, the XGBoost improves the classification accuracy of galaxies in the dark source classification by nearly 10% as compared to the function tree algorithm, and improves the classification accuracy of sources with the darkest magnitudes in the dark source set by nearly 5% as compared to the function tree algorithm. Compared with other traditional machine learning algorithms and deep neural networks, the XGBoost also has different degrees of improvement.     

Status of Satellite Orbit Determination and Time Synchronization Technology for Global Navigation Satellite Systems

In the form of satellite ephemerides and clock parameters, the space datum and system time information of one global navigation satellite system (GNSS) is transferred to users. With the continuous updating in the satellite payload such as the high-precision atomic clock, the monitoring and tracking technique such as the inter-satellite link, and in the data processing technique, the accuracy and real-time performance of the satellite ephemeris and clock error products are steadily improved. Starting from December 27th, 2018, the BeiDou Navigation System 3, or BDS-3, has provided the accurate and reliable basic positioning, navigation, and timing (PNT) service for the users in the countries within the “one belt and one road”. This paper has summarized the faced challenges of the precise orbit determination and time synchronization from the regional BDS-2 system to the BDS-3 global system, and the specific solutions at the control segment. In addition, this paper has compared the BDS with other GNSS systems in terms of technical characteristics. Finally, aiming at a higher accuracy and more reliable PNT service, the road map of precise orbit determination and time synchronization technique for the next generation navigation systems is discussed, which will provide a reference for developing the global navigation satellite systems with an even higher accuracy.     

The Characteristics and Related Problems of the Orbits Around the Earth-Moon Libration Points

Due to the specific dynamics, the probes located at the halo orbits or Lissajous orbits around the Earth-Moon collinear libration point L₁ or L₂ are always studied in the synodic system to understand their trajectories. In fact, they are also orbiting the Earth in a distant Keplerian ellipse. Because of their intrinsic orbital instability, in the orbit prediction the initial errors propagate more prominently than those of the normal orbiting satellites, this requires special attention in the orbit design, maneuver, and control. Despite of all this, they are similar to the normal orbiting satellites in orbit determination and hardly require other special attentions. In this paper, the quantitative results of error propagation under the unstable dynamics, together with the theoretical analysis are presented. The results of precise orbit determination and short-arc orbit predictions are also shown, and compared with the results from the Beijing Aerospace Control Center.     

天文卫星下传数据处理系统的规划

天文卫星获取的数据需要经过卫星下传数据处理系统的一系列加工,生成可以分析的数据产品,这些产品及相应软件要发布给国内外用户,同时数据处理系统还要监测载荷状态、数据质量及天体源爆发等。这样,下传数据处理系统的建设直接关系到物理成果的获取,规划该系统就变得非常有意义。从数据产品定义、子系统规划、数据流程等方面介绍卫星下传数据处理系统的规划,并提出以模块化开发方式从整体上协调各个子系统的开发,使各个系统及其软件相互配合,共同促进科学产出。     

地月系L_2点中继星激光测距成功率的估算

为了模拟位于地月系L2点的中继星"鹊桥"与月球的位置关系,进而估算中继星激光测距的成功率,按照轨道周期约为14天的要求对中继星所在的晕轨道进行计算,建立了一个综合考虑望远镜抖动、大气抖动和预报轨道横向偏离的模型。从数值上给出了一条轨道周期为14. 78天,X方向(地月连线方向)振幅为12 493 km,Y方向为34 596 km,Z方向(垂直于地月轨道平面方向)为11 916 km的周期轨道。由于晕轨道的最小振幅远大于月球遮挡的临界振幅4 000 km,因此月球对中继星不存在遮挡问题。基于建立的测距成功率模型,根据昆明站(国际编号:7820)的激光测距系统对运行在该轨道上的中继星进行测距成功率分析,结果表明:测距成功率随着中继星横向轨道标准差的增大呈快速降低的趋势。对于中继星到测站的平均距离而言,当中继星没有横向偏离时,探测器产生的光电子数为0. 151,成功率为14. 07%;横向偏离2 km时,光电子数降为0. 035,成功率降为3. 46%。对比最近距离与最远距离的情况,无横向偏离的情况下,探测器产生的光电子数从0. 174降为0. 139,成功率从16. 01%降为13. 02%。该计算结果可为云南天文台1. 2 m望远镜实现中继星激光测距提供参考。