Response of Hainan GPS ionospheric scintillations to the different strong magnetic storm conditions

Using the GPS ionospheric scintillation data at Hainan station (19.5°N, 109.1°E) in the eastern Asia equatorial regions and relevant ionospheric and geomagnetic data from July 2003 to June 2005, we investigate the response of L-band ionospheric scintillation activity over this region to different strong magnetic storm conditions (Dst < −100 nT) during the descending phase of the solar cycle. These strong storms and corresponding scintillations mainly took place in winter and summer seasons. When the main phase developed rapidly and reached the maximum near 20–21 LT (LT = UT + 8) after sunset, scintillations might occur in the following recovery phase. When the main phase maximum occurred shortly after midnight near 01–02 LT, following the strong scintillations in the pre-midnight main phase, scintillations might also occur in the post-midnight recovery phase. When the main phase maximum took place after 03 LT to the early morning hours no any scintillation could be observed in the latter of the night. Moreover, when the main phase maximum occurred during the daytime hours, scintillations could also hardly be observed in the following nighttime recovery phase, which might last until the end of recovery phase. Occasionally, scintillations also took place in the initial phase of the storm. During those scintillations associated with the nighttime magnetic storms, the height of F layer base (h’F) was evidently increased. However, the increase of F layer base height does not always cause the occurrence of scintillations, which indicates the complex interaction of various disturbance processes in ionosphere and thermosphere systems during the storms.     

Relative amplitude of the total electron content variations depending on geomagnetic activity

We developed a method of estimation of a relative amplitude dI/I of the total electron content (TEC) variations in the ionosphere as deduced from the data of the global GPS receivers network. To obtain statistically significant results we picked out three latitudinal belts provided in the Internet by the maximum number of GPS sites. They are high-latitudinal belt (50–80°N, 200–300°E; 59 sites), mid latitude belt (20–50°N, 200–300°E; 817 sites), and equatorial belt (±20°N, 0–360°E; 76 sites). The results of the analysis of the diurnal and latitudinal dependencies of dI/I and dI/I distribution probability for 52 days with different levels of geomagnetic activity are presented. It was found that on average the relative amplitude of the TEC variations varies within the range 0–10% proportionally to the value of the K_p geomagnetic index. In quiet conditions the relative amplitude dI/I of the TEC variations at night significantly exceeds the daytime relative amplitude. At high levels of magnetic field disturbances, the geomagnetic control of the amplitude of TEC variations at high and middle latitudes is much more significant than the regular diurnal variations. At the equatorial belt, on average, the amplitude of TEC variations in quiet and disturbed periods almost does not differ. The obtained results may be useful for development of the theory of ionospheric irregularities.     

Influence of the 27-day solar flux variations on the ionosphere parameters measured at Irkutsk in 2003–2005

We present an investigation of the influence of the 27-day solar flux variations, caused by solar rotation, on the ionosphere parameters such as the F2 layer critical frequency (foF2) and the total electron content (TEC). Our observational data were obtained with the Irkutsk Digisonde (DPS-4) located at 52.3 North and 104.3 East during the period from 2003 to 2005. In addition, we use TEC data from the Global Ionosphere Maps (GIM) based on Global Positioning System (GPS) satellites. The solar radiation flux at a wavelength of 10.7 cm (F10.7 index) is used as an index characterizing the solar activity level. A good correlation between observed ionosphere parameters and solar activity variations is found especially in autumn-to-winter season. We estimate the impact of the 27-day solar flux variations on the day-to-day variability and determine the time delay of the ionosphere response.     

中俄联合火星电离层星-星掩星探测

中俄联合火星星-星掩星探测是人类首次在火星空间环境进行此类的联合试验。用于探测火星电离层的星-星掩星技术较以前星地间的探测技术相比,有可接收高信噪比信号,反演精度高,可探测火星上太阳天顶角大于43°,或者小于138°的区域电离层等优点。本文介绍了中俄联合火星星-星掩星探测方案、基本原理,给出了主要技术指标、地面模拟测试结果。     

RCS分析中多次反射的计算及程序实现技术

介绍目标RCS分析计算中多次散射的计算方法,计算多次散射时主要考虑面元-面元之间的相互作用,计算过程采用几何光学法(GO)、物理光学法(PO),在总后向RCS计算中还运用了等效电磁流法.同时,文中讨论计算多次散射的程序实现技术.最后,给出计算例子,考虑多次散射时总的后向RCS计算结果与前人发表的实验结果相吻合.      

两种层板性能对比

针对常规的141型层板,提出了一种增加50％数量扰流柱的设计,即161型层板.采用实验和数值模拟相结合的办法研究了两种类型层板在流阻和换热方面的差别.换热实验部分采用了辐射式加热设备,测量了层板上下表面平均壁温,以及冷气进、出口截面间的焓差,得到了相应进气雷诺数下的层板体积换热努塞尔数.发现161模型流阻降低20％,换热增强5％.对一些实验工况,采用三维计算流体力学程序进行了流-固耦合传热数值模拟,所得结果在趋势上与实验一致,在数值上,流阻和换热与实验结果分别相差5％和30％.利用数值模拟结果分析并比较了两种模型在流场和表面对流换热系数分布方面的细节差别.      

基于SVM的浮动车行驶模式判断模型

浮动车在低速情况下存在两种行驶模式,如不能对上述模式进行准确区分,将严重影响浮动车实时路况计算的精度和效率.研究和设计了一个基于支持向量机(SVM,Support Vector Machine)的浮动车行驶模式判断模型,并针对性地提出了一种简单的基于隶属度矩阵的特征评价和选择方法.实验表明通过上述方法选择的特征子集所训练的分类器在测试样本集上具有92.6%的分类准确性;经过行驶模式分析后,浮动车系统的准确性有显著提升.      

Report on the Kiso cometary dust trail survey

Cometary dust trails were first observed by IRAS; they are widely known to be the origins of meteoric showers. A new window has been opened for the study of dust trails, using ground-based observations. We succeeded in obtaining direct images of the 22P/Kopff dust trail with the Kiso 1.05-m Schmidt telescope. Following this initial success, we have continued to perform a dust trail survey at Kiso. As a result of this survey, we have detected dust trails along the orbit of six periodic comets, between February 2002 and March 2004. The optical depth of these dust trails are 10⁻⁹ to 10⁻⁸, which is consistent with IRAS measurements. In this paper, we describe the observations and data reduction procedures, and report the brief result obtained between February 2002 and March 2004.     

Maxwell方程的高阶间断有限元数值解法

采用高精度方法求解时域Maxwell方程,方程的空间离散采用基于计算流体力学(Computational fluid dynamics,CFD)领域的高阶间断有限元格式,非定常时间迭代采用四步龙格-库塔格式。为了提高计算效率,本文采用了Quadrature-free implementation和网格分区并行技术。数值结果表明,采用高阶格式的情况下,采用稀疏网格便可以得到高精度数值解。另外由于本文的方法基于非结构网格,因此非常适合计算复杂外形的情况。