利用神经网络预报中国地区电离层f0F2

利用神经网络技术并考虑太阳和地磁活动对电离层的影响,提出了一种提前5 h预报中国地区电离层临界频率f0F2的方法.网络输入包括时间、季节、地理纬度、太阳天顶角、最近一天的12个观测值(F-23,F-22,F-21,F-20,F-19,F-18,F-5,F-4,F-3,F-2,F-1,F0)和前30天滑动平均值(A-24,A-23,A-22,A-4,A-3A-2,A-1,A0),网络输出分别为未来5 h的f0F2值F+1,F+2,F+3,F+4,F+5.选取乌鲁木齐、长春、重庆和广州站1958-1968年间的数据训练网络,利用中国9个电离层站的历史数据检验网络,根据均方根误差衡量网络性能的好坏.结果表明,神经网络的预报结果能较好地符合实测数据.这说明利用神经网络实现中国地区电离层f0F2的时空预报是可行的.     

NeQuick模式在亚太地区扇区电离层参数f0F2的预测能力

利用亚洲、澳大利亚地区8个电离层观测台站的F2层临界频率f0F2的历史观测数据,考察了NeQuick模式预报电离层基本参数f0F2在亚太扇区的适应性.对比分析表明,此模式能比较好地预测各地的F2层临界频率,其绝对误差在南半球各站相对北半球各站较大,太阳活动高年相对太阳活动低年较大,春秋季相对夏冬季较大.其误差均方根在太阳活动高年相对太阳活动低年较大.      

低纬(海南)地区电离层偶发E层的潮汐类周期研究

基于低纬(海南)台站(19.5°N,109.1°E)电离层测高仪在2004年观测到的偶发E层(Es)临界频率(f₀E_s)和虚高(h'E_s)数据,利用谱分析方法,给出了中国低纬地区Es层在全年和不同季节内的短周期变化特性.对全年数据谱分析表明,Es层除具有非常强的24h周期外,还具有显著的12h和8h周期.对不同季节内两个参数的谱分析进一步表明,8h周期主要出现在f₀E_s参数的春秋分季和夏末及在h'E_s参数的几乎所有季节;6h周期主要出现在f₀E_s参数的11-12月.海南低纬Es层中具有显著的6h和8h周期特性,特别是这两个周期还能同时出现在冬季,这是以往研究中不曾发现的新结果.初步分析认为,Es层的6h和8h周期极可能是分别由1/4日和1/3日潮汐所造成的.      

顶部电离层总离子密度经度的变化

利用DMSP F13卫星1996-2005年共10年的观测数据,研究地磁中低纬地区黄昏时段(18:00 LT)顶部电离层总离子密度经度变化的季节、地磁纬度和太阳活动变化特征.结果表明总的经度变化在低纬地区与中纬地区具有明显不同特征.不同经度结构的季节变化均以年变化为主,但纬度分布具有明显差异.一波结构主要集中在中纬地区,且南半球明显强于北半球;二波结构南北半球不对称性非常明显;三波结构和四波结构均为低纬地区明显强于中纬地区.通过分析不同波结构对总经度变化的贡献发现,一波结构在南半球中纬地区贡献最大,二波结构在12月前后的15°N附近贡献较大,三波结构和四波结构仅在低纬地区有较强贡献.在不同太阳活动条件下,不同波结构的贡献率有明显变化.      

东亚地区Es特性研究

Es是发生在电离层E层高度上的偶发不规则结构,其电子密度最高可达E层背景电子密度的100倍以上. 远东地区是全球Es的高发区,其相关研究具有独特性和典型性,该地区Es形态学特性的深入研究对于探索Es成因及揭示其本质具有重要意义. 本文利用中国电离层垂测网50余年的垂测数据,结合日本垂测网数据对东亚地区Es的强度特性、空间分布特性、日变化、季节变化以及长期变化趋势进行了深入分析,得到一些有意义的结论.      

中性风对夜间低纬电离层参量的影响

利用一个改进的二维低纬电离层理论模式研究夜间中性风对低纬电离层多量的作用．模式计算结果表明：夜间中性风对低纬F层的影响与纬度、地方时有关．夜间低纬F层峰值电子浓度和峰高及其随时间的变化受中性风的影响与传统观点有所差异．低纬F层参量不只依赖于中性风的方向、强度,还与中性风场空间分布及时间变化率有关．中性风对低纬F层的影响值得重新认识．     

电离层Es对HF和VHF传播信号的影响

Es层是存在于电离层中的电子密度非常高的偶发E层（Sporadic E）,其电子密度可达常规E层的100倍.电离层Es能够反射原本穿透F层的VHF低频段（30~150MHz）无线电波,而且对HF高频段（10~30MHz）无线电波传播具有显著影响.运用垂测和斜测观测数据,研究HF频段Es层电波传播特征,得到了不同类型及不同高度Es层的衰减系数.根据f₀E_s的日变化规律,可得HF频段衰减系数的日变化规律,进而分析并得到Es层对短波传播的影响.不存在电离层Es时,通常无法通过电离层实现VHF超远距离通信.为了对VHF链路通过电离层Es的传播衰减进行定量分析,根据EBU多条链路的观测结果,拟合并建立了电离层Es衰减模型.将该模型、ITU模型和观测数据进行对比,发现本文建立的模型准确度更高.利用建立的模型,对电离层Es不同临频f₀E_s条件下接收信号场强和电压随传播距离的变化进行了计算,结果可为VHF链路设计及建立提供参考.      

地磁场与电离层异常现象及其与地震的关系

利用中国地磁台网与电离层台站资料,总结了大地震前出现的地磁低点位移、地磁日变异常及电离层f0F2(F2层临界频率)异常现象.对比研究了1997年11月8日玛尼7.5级与2001年11月14日昆仑山口西8.1级地震前磁场与电离层异常分布及特征.结果显示,两次巨大地震前磁场与电离层短临异常时空分布特征有较好的一致性,震中周围出现日变异常、拉萨台出现电离层f0F2明显异常;震前约1个月出现地磁低点位移,其突变分界线通过震中地区.      

电离层f_0F_2参数提前24小时预测

利用中国9个垂测站(海口、广州、重庆、拉萨、兰州、北京、乌鲁木齐、长春、满洲里)一个太阳周(1976-1986年)的数据资料,采用三层前向反馈神经网络(BP网络)实现了电离层F2层临界频率(f0F2)参数提前24h预测.通过对f0F2参数的时间序列及其与日地活动之间进行相关分析,确定f(t)(当前时刻f0F2)、经过变换的F10.7指数等5个参数作为神经网络的输入参数,并通过同时段训练法获得不同时刻的预测值,本文与自相关分析法进行了预测性能比较.结果表明,上述方法构建的神经网络可以达到较高的预测精度.针对暴时数据,对神经网络算法进行了改进,提高了神经网络法对暴时数据的适用性.     

中纬地区日间类扩展F不规则结构的观测研究

基于高频多普勒观测,研究中纬地区日间类扩展F现象及其与其他电离层扰动现象的关联.结果表明:日间类扩展F具有出现时间覆盖面广、持续时间长、与其他电离层扰动相互伴随等特征;形态特征表现为回波弥散（与夜间扩展F相似）,弥散回波的频移多倾向于正向偏移,有时与行进电离层扰动（TIDs）相互伴随.日间类扩展F现象虽然是偶发事件,且发生率极低,但其出现时间及区域的广泛性充分体现了该现象对空间天气及空间环境的影响具有不可忽视的重要性.      

Prompt effects of solar wind variations on the inner magnetosphere and midlatitude ionosphere

It is well known that the solar wind can significantly affect high-latitude ionospheric dynamics. However, the effects of the solar wind on the middle- and low-latitude ionosphere are much less studied. In this paper, we report observations that large perturbations in the middle- and low-latitude ionosphere are well correlated with solar wind variations. In one event, a significant (20–30%) decrease of the midlatitude ionospheric electron density over a large latitudinal range was related to a sudden drop in the solar wind pressure and a northward turning of the interplanetary magnetic field, and the density decrease became larger at lower latitudes. In another event, periodic perturbations in the dayside equatorial ionospheric E × B drift and electrojet were closely associated with variations in the interplanetary electric field. Since the solar wind is always changing with time, it can be a very important and common source of ionospheric perturbations at middle- and low-latitudes. The relationship between solar wind variations and significant ionospheric perturbations has important applications in space weather.     

Recent Progresses on Ionospheric Climatology Investigations

The ionosphere varies over multiple time scales, which are classified into two categories: the climatology and weather variations. In this national report, we give a brief summary of recent progresses in ionospheric climatology with focus on (1) the seasonal variations, (2) solar cycle effects, and (3) empirical modeling of the ionosphere. The seasonal variations of the ionosphere have been explored in many works to give a more detailed picture with regional and global features at various altitudes by analyzing the observation data from various sources and models. Moreover, a series of studies reported the response of the ionosphere to solar cycle variations, which revealed some novel and detailed features of solar activity dependence of ionospheric parameters at different altitudes. These investigations have improved our understanding on the states of the ionosphere and underlying fundamental processes, provided clues to future studies on ionospheric weather, and guided ionospheric modeling, forecasting and related applications.      

Variations of quasi-electrostatic fields and ionosphere potential above lightning discharge at equatorial latitudes

Lightning discharges by thunderstorms cause generation of electromagnetic pulses and of quasi-electrostatic fields (QESF) in the atmosphere above, which occur in different time-scales. QESF penetrate into the mesosphere and the lower ionosphere where they are big enough to generate considerable electric charge transfer there and, in some cases, to cause red sprites. These processes may have an important contribution to the global atmospheric electric circuit. Significant transient variations of the ionospheric potential above the thunderstorm take place as well. QESF depend on the atmospheric conductivity and in the ionosphere they are affected also by its anisotropy determined by geomagnetic field orientation. QESF after a lightning discharge are investigated theoretically in this work in the case of equatorial latitudes (by horizontal geomagnetic field), where thunderstorms are important contributors to the global circuit. Results for DC electric fields in the lower equatorial ionosphere above a thundercloud obtained by earlier models demonstrate some specific features of the spatial distribution of these fields, which appear due to geomagnetic field orientation. Thus, the electric fields can be shifted by tens or more kilometers to east of the cloud charge region; also their horizontal scale is much bigger than in the case of middle latitudes. Here, a presence of similar specific features of quasi-electrostatic field distributions and ionospheric potential variations caused by a lightning stroke is studied. A situation when no secondary ionization is generated is considered. A model based on the Maxwell equations for potential electric fields is proposed. Computations of QESF in the middle atmosphere and of the ionospheric potential variations are provided as dependent on conductivity and its anisotropy in D-region. The obtained results for the ionosphere show that the electric fields in the equatorial lower ionosphere are comparable to these formed in the case of middle latitudes. However, their horizontal scales are much bigger and depend on conductivity profiles. Similar features are valid also for the ionospheric potential variations and for their horizontal scales.     

Electron densities and temperatures in the Venus ionosphere: Effects of solar EUV,solar wind pressure and magnetic field

The Venus ionosphere is influenced by variations in both solar EUV flux and solar wind conditions. On the dayside the location of the topside of the ionosphere, the ionopause, is controlled by solar wind dynamic pressure. Within the dayside ionosphere, however, electron density is affected mainly by solar EUV variations, and is relatively unaffected by solar wind variations and associated magnetic fields induced within the ionosphere. The existence of a substantial nightside ionosphere of Venus is thought to be due to the rapid nightward transport of dayside ionospheric plasma across the terminator. Typical solar wind conditions do not strongly affect this transport and consequently have little direct influence on nightside ionospheric conditions, except on occasions of extremely high solar wind dynamic pressure. However, both nightside electron density and temperature are affected by the presence of magnetic field, as in the case of ionospheric holes.     

The solar wind control of the equatorial ionosphere dynamics during geomagnetic storms

The interplanetary magnetic field, geomagnetic variations, virtual ionosphere height h′F, and the critical frequency foF2 data during the geomagnetic storms are studied to demonstrate relationships between these phenomena. We study 5-min ionospheric variations using the first Western Pacific Ionosphere Campaign (1998–1999) observations, 5-min interplanetary magnetic field (IMF) and 5-min auroral electrojets data during a moderate geomagnetic storm. These data allowed us to demonstrate that the auroral and the equatorial ionospheric phenomena are developed practically simultaneously. Hourly average of the ionospheric foF2 and h′F variations at near equatorial stations during a similar storm show the same behavior. We suppose this is due to interaction between electric fields of the auroral and the equatorial ionosphere during geomagnetic storms. It is shown that the low-latitude ionosphere dynamics during these moderate storms was defined by the southward direction of the B_z-component of the interplanetary magnetic field. A southward IMF produces the Region I and Region II field-aligned currents (FAC) and polar electrojet current systems. We assume that the short-term ionospheric variations during geomagnetic storms can be explained mainly by the electric field of the FAC. The electric fields of the field-aligned currents can penetrate throughout the mid-latitude ionosphere to the equator and may serve as a coupling agent between the auroral and the equatorial ionosphere.     

The high-latitude ionosphere structure on 22 March, 1979 magnetic storm from multi-satellite and ground-based observation

Variations in the high-latitude ionosphere structure during March 22, 1979 geomagnetic storm are examined. Electron density Ne and temperature Te from the Cosmos-900 satellite, NmF2, Ne and He⁺ from the ISS-b satellite, precipitation of soft electrons from the Intercosmos-19 satellite, and the global picture of the auroral electron precipitation from the DMSP, TIROS and P78 satellites are used. These multi-satellite databases allow us to investigate the storm-time variations in the locations of the following ionospheric structures: the day-time cusp, the equatorial boundary of the diffuse auroral precipitation (DPB), the main ionospheric trough (MIT), the day-time trough, the ring ionospheric trough (RIT) and the light ions trough (LIT). The variations in NmF2, Ne, He⁺ and Te in the high-latitude ionosphere for the different local time sectors are analyzed also. The features of the high-latitude ionospheric response to a strong magnetic storm are described.     

释放SF6气体扰动电离层时的人工气辉研究

在电离层高度释放SF₆气体能够显著扰动电离层.根据SF₆分子在电离层中的扩散方程,同时考虑其在电离层中主要的离子化学反应,研究了SF₆气体释放后电离层各粒子浓度的时空变化,计算了产生人工气辉的体发射系数和发射强度.结果表明,SF₆气体在电离层高度释放后,电子和O⁺的密度均有大幅度下降,主要的负离子成分由电子转变成SF₅^-;在释放过程中,主要产生777.4 nm和135.6 nm两种气辉,且前者的气辉强度远小于后者;电离层温度对气辉的强度有很大的影响.本文的数值计算与美国IMS/SF₆实验观测数据进行比较,结果近似,且通过数据比较还能准确推断出实验时当地的电离层温度.     

Fading in the HF ionospheric channel and the role of irregularities

It is well known that the ionosphere affects radio wave propagation especially in the high frequency (HF) range. HF radio waves reflected by the ionosphere can reach considerable distances, often with changes in amplitude, phase, and frequency. The ionosphere is a dispersive in frequency and time, bi-refractive, absorbing medium, in which multipath propagation due to traveling irregularities is very frequent. The traveling irregularities undulate the reflecting ionospheric layer, introducing variations in signal amplitude (fading). In this multipath time variant channel fading is mainly considered, even though it is not the sole effect. Echo signals from a single reflection, as in ionospheric vertical sounding (VIS) techniques, are affected by a certain degree of variability even in quiet ionospheric conditions. In this work the behavior of the ionospheric channel is studied and characterized by observing the power variation of received echoes using the VIS technique. Multipath fading was analyzed quantifying the power variation of the signal echo due to irregularities on a temporal scale from 0.5 to 256 s. An experimental set-up derived from an ionosonde was implemented and the analysis was performed employing a special numerical algorithm operating off-line on the acquired time sequence of the signal. The gain-loss of the irregularity shapes are determined in some special cases.     

An annual variation analysis of the ionospheric spatial gradient over a regional area for GNSS applications

An ionospheric spatial gradient represents the ionosphere delay difference between different locations, and its variation over a specific area is important for implementing differential GNSS systems. An estimation method for the ionospheric spatial gradient over a small regional area is proposed. A plate map model is implemented for the direct estimation of the gradients. Nine years of GPS data were processed to figure out the annual variation of the mean gradient at the mid-geomagnetic latitude of 30° N. Gradients along the north–south direction have a mean of 0.65 mm/km and follow solar-cycle variations.     

电离层周日变化对解算GPS硬件延迟稳定性的影响

针对电离层周日变化特征分析了其可能对SCORE方法估算的硬件延迟稳定性的影响. 利用BJFS以及XIAM台站的GPS观测数据, 解算了位于太阳活动高年(2001年)和太阳活动低年(2009年)的卫星硬件延迟并分析了估算的硬件延迟的稳定性. 研究发现, 电离层周日变化对估算的硬件延迟稳定性具有一定影响, 但是利用不同台站所得到的卫星硬件延迟稳定性在昼夜不同时间上的解算结果存在一定差异. 电离层周日变化对利用 BJFS台站数据解算的硬件延迟稳定性日夜差异较为明显, 在太阳活动高年利用XIAM 台站数据解算的硬件延迟日夜稳定性差异不很明显, 由于XIAM台站处于电离层赤道异常峰附近, 夜间电离层变化很大, 因此对比中纬度地区, 电离层周日变化对赤道异常峰附近地区硬件延迟稳定性解算结果的影响相对较小, 但在太阳活动低年, 其影响仍较为显著.