基于Swarm卫星GPS/TEC观测的顶部电离层三维电子密度分布的层析法研究

利用两颗伴飞的Swarm A/C卫星搭载的双频GPS接收机获取的TEC数据,在两个卫星轨道平面同时对顶部电离层电子密度进行层析成像,实现对顶部电离层电子密度的三维观测.为了能够重现扰动期间电离层电子密度的空间变化特征,在正则化求解过程中,我们引入了水平矩阵H和垂直矩阵V刻画电子密度的空间变化特征,引入整体约束矩阵C以调节不同空间对电子密度相对变化的权重.数值验证结果表明我们的算法对常见的观测误差具有较强的包容性,反演计算出的电子密度平均偏差优于10%.在不同地磁活动条件下,与第三方观测数据的对比,验证了本文反演算法的可靠性.实测数据反演结果表明我们的算法不仅能够较好地重现顶部电离层子午向百公里级别的不规则结构,还能有效分辨纬向相隔～150 km的两个卫星轨道平面的电子密度差异.     

顶部电离层和等离子体层电子密度分布——基于GRACE星载GPS信标测量的CT反演

本文利用两颗跟飞的GRACE卫星载GPS信标测量数据和基于差分相对TEC的层析算法,实现了全球范围的顶部电离层和等离子体层(450~5000 km) 层析成像.反演结果表明,利用低轨道卫星载GPS信标测量数据可以有效地重建顶部电离层和等离子体层的全球二维分布图像.对不同地磁活动条件下的天基层析反演结果表明,等离子体层电子密度随纬度的分布是不均匀的;在低纬赤道带,从顶部电离层向上延伸直到等离子体层,以及等离子体层中局地的电离增强云团,经常出现近似垂直于磁力线的电子密度柱状增强结构.     

基于选权拟合法的电离层电子密度层析重构

附加约束的电离层层析算法是解决电离层电子密度反演中不适定问题的主要方法,为避免此类方法中约束权阵的选取不当对电子密度分布重构产生的不良影响,本文将选权拟合法应用到电离层层析成像技术中.该方法特别设计了依据电子密度空间分布特性构造参数权矩阵的方案.新方法有明确的物理意义,挖掘了隐含的信息量,为解决电离层电子密度反演中由于观测数据的不足等因素引起的不适定问题提供了一种新途径,可以得到符合客观实际的结果.数值模拟实验和实测数据的反演结果证实了该算法有效性、可靠性和优越性.     

远紫外光谱遥感反演电离层EDP技术

本研究基于美国GUVI观测氧原子135.6 nm夜气辉光谱数据,建立了GUVI临边观测模型,采用正则化和牛顿迭代法相结合的方法,消除了权重矩阵的病态问题,得到了峰值电子密度和峰值高度,并结合电离层电子密度的Chapman表达式,反演得到了电离层电子密度剖面.将得到的反演结果与地基方式获取的观测数据进行比较,两者吻合得很好.之后,反演得到了磁暴期2002年9月29日到10月3日的电子密度剖面,初步分析了电离层电子密度剖面随磁暴的变化情况.     

三维模式约束的电离层掩星反演方法

目前电离层掩星数据反演是基于电离层电子密度分布局部球对称近似的Abel反演方法,实际电离层的非球对称性会给电子密度反演结果带来误差.本文研究利用三维电离层模式来提供电子密度水平变化的先验信息约束电离层掩星反演的方法,即三维模式约束法;并将该方法应用于模拟掩星观测数据和实测掩星数据的反演.模拟观测数据的反演结果表明,与Abel反演方法相比,三维模式约束法能够减小反演误差.采用IRI2001模式作为约束,对COSMIC电离层掩星实测数据反演,将反演结果与全球的垂测仪数据进行比较,结果表明,三维模式约束法和Abel反演方法都能很好地反演电离层掩星.     

GPS地面台网和掩星观测结合的时变三维电离层层析

本文给出GPS地面台网和掩星观测结合的时变三维电离层层析的原理、算法和基于实测数据的反演结果.反演结果的比较表明,联合地基GPS与掩星观测数据进行重建,电子密度整体图像的重建质量特别是其垂直结构的重建质量得到了明显改善.在平静日和磁暴期间两种条件下利用实测数据的重建结果表明,GPS地面台网和掩星观测结合的电离层层析可以获得电离层电子密度在高度-纬度-经度-时间四维空间中的变化.重建结果清晰地显示了磁暴期间电离层负相暴效应,表明结合GPS地面台网和掩星观测的时变三维电离层层析可以有效地监测扰动条件下的大尺度电离层结构.     

电离层三维层析成像的自适应联合迭代重构算法

在电离层层析成像过程中,联合迭代重构算法是一种常用的反演算法.然而,该算法迭代收敛较慢,反演结果精度不高.为此,本文发展了一种自适应的联合迭代重构算法,该算法利用上一轮的电离层电子密度反演结果,自适应地调整松弛因子和加权参数.通过模拟数据和实测数据对该算法的反演结果进行了验证,并将得到的反演结果与电离层测高仪数据进行了比较,结果表明,该算法能够有效地反演电离层电子密度,且反演结果精度优于常用的联合迭代重构算法.     

一种基于LEO卫星信标的电离层层析成像新算法

LEO卫星信标是电离层监测的重要手段之一.利用电离层层析成像算法,LEO卫星信标能够实现区域电离层电子密度的快速重构.针对LEO卫星信标的特点,本文提出了一种函数基模型与像素基模型组合的电离层层析成像新算法.选择差分相对电离层总电子含量作为输入数据源,先通过函数基模型法获取电离层电子密度初始分布,再利用像素基模型法对初始分布进行二次迭代重构,该方法可有效降低电离层层析成像对背景电离层模型的依赖,同时能够实现电离层小尺度扰动结构的有效反演.利用数值仿真方法及低纬度电离层层析成像网的实测数据的反演结果验证了本文提出的新算法的可行性和可靠性.     

电离层GPS掩星观测改正TEC反演方法

电离层掩星观测中，当低轨卫星（LEO）轨道高度较低时，轨道以上的电离层电子总含量（TEC）对掩星反演的影响不能忽略.目前，一般采用指数函数等外推方法来处理该问题，对反演结果可能引起较大误差.为提高电离层掩星反演精度，本文研究利用LEO处于非掩星一侧GPS观测数据的改正TEC新反演方法.用三维射线追踪程序计算出电离层掩星观测模拟数据，分别应用改正TEC方法和外推方法进行反演，将反演结果与所用模式值进行比较.结果表明：对于轨道高度约800km的GPS/MET掩星模拟数据，外推方法和改正TEC方法反演结果都与模式值基本一致；对于轨道高度约400km的CHAMP掩星模拟数据，外推方法误差较大，改正TEC方法反演结果与模式值相符得较好.将改正TEC方法应用于GPS/MET实测数据的反演，取得了合理的结果.这些说明，改正TEC算法是一种有效的电离层掩星反演方法，尤其是对于轨道较低的LEO的电离层掩星观测反演特别有用.     

基于Swarm卫星数据的一次地震电离层现象辨识

为进一步探索基于多颗卫星观测数据的地震电离层现象识别,利用Swarm星座三颗卫星观测的电子密度数据和磁场数据,对已报道的2017年11月12日伊朗M_W7.3地震震前第9天震中附近的一次地震电离层扰动现象进行辨识。通过分析三颗卫星相邻轨道的电离层扰动特征,获得了异常扰动存在的空间范围;利用Swarm星座三颗卫星轨道的时间和空间差异,计算出异常扰动在空间中可能的传播特征;使用同步观测的磁场数据判断其电磁辐射特性。最终根据现有对地震电离层耦合的认知,并结合分析的结果,认为该扰动为非震源发出的声重波扰动,非沿纬向传播的电离层行波扰动,非同步电磁辐射引发扰动,而是与伊朗M_W7.3地震孕育活动无关的一次高纬度强烈电离层活动所引起的扰动变化。      

Reconstructing Regional Ionospheric Electron Density: A Combined Spherical Slepian Function and Empirical Orthogonal Function Approach

The computerized ionospheric tomography is a method for imaging the Earth’s ionosphere using a sounding technique and computing the slant total electron content (STEC) values from data of the global positioning system (GPS). The most common approach for ionospheric tomography is the voxel-based model, in which (1) the ionosphere is divided into voxels, (2) the STEC is then measured along (many) satellite signal paths, and finally (3) an inversion procedure is applied to reconstruct the electron density distribution of the ionosphere. In this study, a computationally efficient approach is introduced, which improves the inversion procedure of step 3. Our proposed method combines the empirical orthogonal function and the spherical Slepian base functions to describe the vertical and horizontal distribution of electron density, respectively. Thus, it can be applied on regional and global case studies. Numerical application is demonstrated using the ground-based GPS data over South America. Our results are validated against ionospheric tomography obtained from the constellation observing system for meteorology, ionosphere, and climate (COSMIC) observations and the global ionosphere map estimated by international centers, as well as by comparison with STEC derived from independent GPS stations. Using the proposed approach, we find that while using 30 GPS measurements in South America, one can achieve comparable accuracy with those from COSMIC data within the reported accuracy (1 × 10¹¹ el/cm³) of the product. Comparisons with real observations of two GPS stations indicate an absolute difference is less than 2 TECU (where 1 total electron content unit, TECU, is 10¹⁶ electrons/m²).     

磁暴期间高纬顶部电离层离子上行特征——DMSP卫星观测

本文利用DMSP F13和F15卫星观测数据,对2001—2005年58个磁暴(-472 nT≤Min.Dst≤-71 nT)期间高纬顶部电离层离子整体上行特征进行了统计研究.观测表明,磁暴期间,顶部电离层离子上行主要发生在极尖区和夜间极光椭圆区.在北半球,磁正午前,高速的离子上行(≥500 m·s^-1)多集中在65° MLat以上;午后,高速离子上行区向低纬度扩展,上行速度要略高于午前;在南半球,磁午夜前,DMSP卫星在考察区域内几乎所有的纬度上都观测到了高速上行的离子;午夜后,各纬度上观测到上行离子的速度明显降低.离子上行期间,DMSP卫星在极区顶部电离层高度上也频繁地观测到电子/离子增温,且电子增温发生的频率要远高于离子增温.O⁺密度变化分析显示,DMSP卫星磁暴期间观测到的上行离子更多地源于顶部电离层高度.这些结果表明电子增温在驱动暴时电离层离子整体上行过程中起着重要作用.     

地球等离子体层及EUV遥感测量技术

地球等离子体层位于地球电离层以上,延伸至4~6地球半径范围的环状等离子体区域,它在空间分布上与地球辐射带、环电流区域重合,是地球内磁层研究的重要内容。本文综述了地球等离子体层遥测技术的原理、发展,并总结和分析了EUV-CT的现有成果。      

Ionospheric response to the extreme solar burst of October 28, 2003

Using GPS and GLONASS navigation systems, instantaneous observations of solar burst effects on the Earth’s ionosphere are made. These observations are carried out for both Northern and Southern hemispheres, including the ionosphere at polar and equatorial latitudes. It is shown that the rate of total electron content (TEC) change is agrees well with the time profiles of solar bursts. An experimental dependence of the electron content gradient on the elevation angle is obtained.     

Observations of subterahertz radiation of solar flares with an RT-7.5 radiotelescope

We analyzed unique observations of two flare events at frequencies of 93 and 140 GHz. The observations were carried out with an RT-7.5 radiotelescope at the Bauman State Technical University (Moscow) using the method of continuous active region tracking with spatial resolutions of 2.5 (at a frequency of 93 GHz) and 1.5 arc-minutes (at 140 GHz). The light curves of the bursts were analyzed and compared with the time profiles of soft and hard X-ray emission obtained by the GOES and RHESSI spacecraft. The radio delete this word flux density spectra were plotted. It was found that the radiation flux at a frequency of 140 GHz exceeded the flux at 93 GHz. This constitutes a new independent confirmation of the presence of a subterahertz flare component, the appearance of which may be associated with the thermal radiation of the hot plasma at the base of flare loops.     

The concentration of negative ions of oxygen and its combinations in the ionosphere

Summary There are some processes in the ionosphere which were or could be explained by means of negative ions, such as sunrise effects, echo duration anomalies of meteor train radar observations and others. Therefore the concentration of negative ions was computed in this paper for some electron density distributions in a stationary quasineutral model of the undisturbed ionosphere. Such an investigation seems necessary because in the last few years laboratory experiments and theoretical calculations give some improved values of attachment and detachment coefficients. The density of negative ions at 12 00 local time and at 00 00 local time in dependence on height was calculated. A discussion of these values shows that negative ions must be considered only in the lower ionosphere at most up to 130 km. This agrees well with the conclusions derived from the observations. By using the values derived in this paper it seems possible to explain some results of ionosphere measurements such as those concerning sunrise effects and others.Mitteilung Nr. 124.     

An upgrade of the solar-wind-driven empirical model for the middle latitude ionospheric storm-time response

Based on recent advances in ionospheric storm dynamics that correlate the ionospheric storm effects with space weather parameters such as the magnitude of the interplanetary magnetic field (IMF), its rate of change and the IMF's orientation in the north–south direction and on the availability of these parameters in real time by NASA ACE spacecraft from the vantage L1 point, an empirical storm-time ionospheric model for the middle latitude ionosphere, namely STIM, was recently envisaged. STIM is significantly upgraded and validated here. The model introduces a correction factor to the quiet daily ionospheric variation to anticipate storm conditions. It is triggered by an alert signal for upcoming ionospheric disturbances obtained from the analysis of the IMF measurements provided by ACE spacecraft. In its final version, STIM method includes quantitative criteria for the online analysis of the ACE's observations. The determination of the ionospheric storm onset and the empirical formulation of the ionospheric storm-time response, both in terms of the local time and the latitude of the observation point are also specified here. STIM's forecasts are provided from 13 to 45 h ahead for any middle latitude ionospheric location. Validation tests carried out for 27 storm-time intervals and for four European locations show that the model captures successfully the onset and the recovery of the ionospheric disturbance and follows sufficiently the disturbance pattern, providing also significant improvement over climatology during storm days. STIM was also compared with two well-known prediction models, the IRI2001 and the GCAM, and the findings demonstrate improved performance in favour of STIM, in both quantitative and qualitative aspect. In general, the results presented here support the efficiency of the proposed methodology in providing reliable ionospheric forecasts at middle latitudes several hours in advance. The operational implementation of STIM can support ionospheric forecasting space weather services and is based on the availability of real-time IMF observations from the vantage L1 point.     

MHD model of magnetosheath flow: comparison with AMPTE/IRM observations on 24 October, 1985

We compare numerical results obtained from a steady-state MHD model of solar wind flow past the terrestrial magnetosphere with documented observations made by the AMPTE/IRM spacecraft on 24 October, 1985, during an inbound crossing of the magnetosheath. Observations indicate that steady conditions prevailed during this about 4 hour-long crossing. The magnetic shear at spacecraft entry into the magnetosphere was 15°. A steady density decrease and a concomitant magnetic field pile-up were observed during the 40 min interval just preceding the magnetopause crossing. In this plasma depletion layer (1) the plasma beta dropped to values below unity; (2) the flow speed tangential to the magnetopause was enhanced; and (3) the local magnetic field and velocity vectors became increasingly more orthogonal to each other as the magnetopause was approached (Phan et al., 1994). We model parameter variations along a spacecraft orbit approximating that of AMPTE/IRM, which was at slightly southern GSE latitudes and about 1.5 h postnoon Local Time. We model the magnetopause as a tangential discontinuity, as suggested by the observations, and take as input solar wind parameters those measured by AMPTE/IRM just prior to its bow shock crossing. We find that computed field and plasma profiles across the magnetosheath and plasma depletion layer match all observations closely. Theoretical predictions on stagnation line flow near this low-shear magnetopause are confirmed by the experimental findings. Our theory does not give, and the data on this pass do not show, any localized density enhancements in the inner magnetosheath region just outside the plasma depletion layer.