基于GNSS观测的全球赤道等离子体泡对太阳和地磁活动及季节依赖特征

赤道等离子体泡是在磁赤道和低纬地区一种通常发生在夜间的大尺度电离层不规则结构.本文利用2010—2021年全球低纬地区GNSS TEC监测仪长期观测数据,分析了赤道等离子体泡对太阳和地磁活动及季节的依赖特征.结果表明,全球每个经度区赤道等离子体泡发生率与太阳活动都显著正相关,赤道等离子体泡的日发生率与F₁₀₇指数相关系数接近0.70.经度-60°～-30°在赤道等离子体泡高发月份的日落后发生率与F₁₀₇的相关关系有明显的饱和效应.在季节变化方面,经度-60°～-30°赤道等离子体泡主要发生在1—3月和10—12月,其他经度主要发生在分季.不同经度区赤道等离子体泡日落后发生率季节不对称性存在显著区别,在太阳活动上升期,经度-60°～-30°的10—12月发生率明显高于1—3月;在太阳活动下降期,0°～180°经度区3月分季高于9月分季.此外,地磁扰动对产生赤道等离子体泡主要是抑制作用,特别是在太阳活动高年、分季.     

利用卫星和GPS观测研究低纬局部等离子体浓度增强现象

本文同时利用DMSP、ROCSAT-1卫星数据和地基的GPS观测数据,研究一种与低纬等离子体泡相伴随的局部等离子体浓度增强现象.地基GPS的观测表明电离层总电子含量(TEC)也能反映这种等离子体浓度增强.通过4个观测事例的详细分析表明:这种等离子体浓度增强主要出现在磁纬±10°～±20°的局部区域,有时在近磁赤道区和中纬地区的电离层顶部也能观测到;与等离子体泡的出现规律相似,这种等离子体浓度增强主要出现在地方时21∶00以后,并在午夜后也能观测到.当等离子体浓度增强和等离子体泡发生时,在午夜前一般对应着背景垂直速度明显向上的扰动,在午夜后一般处于等离子体垂直速度下降至反向前的时间段,表明东向电场对于低纬不规则体的产生有非常重要的作用.     

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.     

磁宁静期核心等离子体层电子密度分布的统计研究

等离子体层已有数十年研究历史,但对其核心等离子体区域却一直没有一个相对准确的界限和模型定义.基于范阿伦辐射带卫星RBSP-A在2012年9月18日至2014年10月13日约两年的观测,我们统计研究了磁宁静期间核心等离子体层电子密度随磁地方时(MLT)及磁壳指数(L-value)的分布特征.发现了核心等离子体层电子密度在不同MLT条件下随L值的变化趋势几乎一致,但与以前的等离子体层经验模式计算的电子密度存在较大的偏差.在不同L值下电子密度随MLT的变化趋势也相差不大,而且随MLT存在明显的逐日和半日变化.最后我们获得了等离子体层电子密度随L值和MLT变化的经验公式.研究结果对空间等离子体层建模及研究具有重要的意义.     

日侧伴随电子加速的离子上行事件的分布特征

本文基于2005年1月和7月DMSP F13卫星的观测数据,研究了日侧伴随电子加速的顶部电离层离子整体上行事件的分布特征.结果表明,离子上行主要发生在磁纬70°～80°MLAT范围内,加速电子磁层源区对应低纬边界层和等离子体片边界层;冬季上行存在明显的“晨昏不对称性”,主要发生在晨侧(06∶00—09∶00 MLT),夏季上行主要发生在磁正午(09∶00—15∶00 MLT),以磁正午为中心近似呈对称分布,并且冬季离子上行发生率显著高于夏季;离子上行发生率在中等地磁活动时期显著增强,上行区域随着地磁活动的增强向低纬度方向扩展;行星际磁场B_x>0时,对应等离子体片边界层13∶00—18∶00 MLT和06∶00—09∶00 MLT区域内上行发生率增加,行星际磁场B_y的方向会导致上行高发区以磁正午为中心发生反转,行星际磁场南向时,上行发生率增强;冬季离子上行平均速度高于夏季.     

基于非相干散射雷达和GPS观测研究Millstone Hill地区等离子体层电子含量

本文尝试结合非相干散射雷达和GPS TEC观测数据提取等离子体层总电子含量(PTEC).我们首先描述所用的技术方法,然后具体利用了Millstone Hill台站的观测数据研究该地区上空等离子体层总电子含量(PTEC)的变化情况.我们采用变化标高的Chapman函数对非相干散射雷达测得的电子浓度剖面数据进行拟合,然后通过对剖面积分得到100 km到1000 km高度范围的电离层总电子含量.GPS提供的TEC数据为高度达20200 km的总电子含量,两者之差可近似看成等离子体层的电子含量.本文分别选取太阳活动高年(2000, 2002年)和太阳活动低年(2005,2008年)Millstone Hill台站的静日数据进行研究.结果表明,等离子体层电子含量及其所占GPS TEC的比例具有明显的周日变化.PTEC含量在白天高于夜间,而所占GPS TEC的百分比,夜间明显高于白天.太阳活动高年所选月份等离子体层电子含量在4~14 TECU (1TECU=10¹⁶el/m²) 范围内变化,夜间所占比例可达60%左右.太阳活动低年所选月份等离子体层电子含量在3~7 TECU范围内变化,所占比例夜间最高可达80%左右.我们所得到的结果与前人基于其它观测手段所得结果在变化趋势上一致,在量级上也大致相当.因此,这从一个侧面证明了我们所用方法的可靠性.非相干散射雷达能够探测包括F2层峰值以下及以上高度的电子浓度,利用这一设备所观测得到的资料来推算电离层电子含量将比前人基于电离层垂测仪观测资料进行的推算更具真实性,由此得到的等离子体层电子含量也将更为接近真实情况.     

2020年8月18日印度尼西亚MS7.0地震电离层扰动研究

基于GPS TEC单站数据、 GIM TEC数据、垂测数据以及中国电磁监测试验卫星观测的原位电子密度数据,利用时序和空间的扰动提取方法,对2020年8月18日(世界时)印度尼西亚M_S7.0地震所引起的电离层扰动开展了研究。通过分析,我们发现多数据源的异常主要集中出现在8月12日—8月15日。震中附近8月12日GPS TEC单站数据和GIM TEC数据有明显的正异常现象,8月13日卫星原位电子密度和GIM TEC数据提取到正异常扰动,8月14日观测到卫星原位电子密度和GPS单站TEC数值有所增加,8月15日卫星原位电子密度、 GIM TEC和GPS单站TEC均出现正异常现象。此次地震引起的电离层异常不仅出现在震中上空,同时也反映在震中磁共轭区域。对应于8月12日震中附近的TEC异常,磁共轭区的单站TEC出现同步扰动,8月13日卫星数据、 GIM TEC和单站TEC数据在磁共轭区同步响应,8月15日磁共轭区的卫星原位电子密度、 GIM TEC、 GPS单站TEC和垂测数据均提取到了正异常扰动,并且与震中附近扰动出现的时间和幅度都有一定的共性。     

2004年11月强磁暴期间武汉电离层TEC的响应和振幅闪烁特征的GPS观测

本文利用设在武汉(11436°E,3053°N,磁纬194°)的GPS电离层TEC和电波闪烁监测仪的测量数据,分析了2004年11月强磁暴期间TEC的响应以及电波闪烁和TEC起伏的特征.结果表明,在这次强磁暴期间,武汉及其邻近地区电离层TEC的响应以正暴相为主,正暴相分别出现在两次主相期间,最大正偏离达到50 TECU.这次磁暴另一个重要影响是主相期间L波段振幅闪烁的活动性及其强度显著增强.S4指数最大接近10.伴随增强的闪烁活动,多次观测到深度耗尽的等离子体泡与TEC起伏,TEC变化率的标准差ROTI指数也显著增强.分析揭示, ROTI指数与S4指数呈正相关,相关系数达到097.线性回归计算得到,ROTI和S4的比率为964.     

基于三亚VHF雷达的场向不规则体观测研究:4.太阳活动低年夏季F区回波

太阳活动低年夏季,低纬电离层F区场向不规则体表现出与太阳活动高年和其他季节明显不同的特征.本文利用我国三亚站(18.4°N,109.6°E,地磁倾角纬度dip latitude 12.8°N)VHF雷达、电离层测高仪、GPS闪烁监测仪和美国C/NOFS卫星观测数据,研究了太阳活动低年夏季我国低纬电离层F区场向不规则体的基本特征.分析发现无论磁静日还是磁扰日,夏季电离层F区不规则体回波主要出现于地方时午夜以后,回波出现的时间较短,高度范围较小,伴随着扩展F出现,但没有同时段的L波段电离层闪烁.太阳活动低年夏季午夜后的低纬电离层F区不规则体回波,可能并不总是与赤道等离子体泡沿磁力线向低纬地区的延伸相关,而可能由本地Es等扰动过程引起.     

基于注意力机制LSTM的电离层TEC预测

电离层总电子含量(Total Electron Content, TEC)的监测与预报是空间环境研究的重要内容,对卫星通讯和导航定位等有重要意义.TEC值影响因素较多,很难确定精确物理模型来对其进行预测.本文设计了基于注意力机制的LSTM模型(Att-LSTM),采用过去24小时TEC观测数据对未来TEC进行预测.选择北半球东经100°上,每2.5°纬度选择一个位置,共计36个位置来验证本文提出模型的性能,并与主流的深度学习模型如DNN、RNN、LSTM进行对比实验.取得了如下成果：(1)在选定的36个地区未来2小时单点预测上,基于本文的Att-LSTM模型的TEC预测性能明显优于其他对比模型;(2)讨论了纬度对Att-LSTM预测未来2小时TEC值时性能的影响,发现在北纬0°到60°之间,Att-LSTM预测性能随着纬度的升高而略有降低,在北纬62.5°～87.5°之间,模型预测性能出现扰动,预测效果略差;(3)讨论了磁暴期和磁静期模型的预测性能,发现无论是磁暴期还是磁静期,本文模型预测性能均较好;(4)还讨论了对未来多时点预测效果,实验结果表明,本文所提出的模型对未来2、4个小时的...     

Plasmaspheric electron content (PEC) over low latitude regions around the magnetic equator in the Indian sector during different geophysical conditions

The variation of plasmaspheric electron content (PEC) is an important parameter for studying the effects of space weather events in the low latitude ionosphere. In the present study, the vertical TEC (VTEC) measurements obtained from co-located dual-frequency Global Positioning System (GPS) and Coherent Radio Beacon Experiment (CRABEX) systems have been used. The daytime PEC variations under different geophysical conditions have been estimated (around the magnetic equator) over the Indian sector, for the first time. The first observations of the nighttime PEC variations over the Indian sector are also estimated from the simultaneous measurements of Faraday rotation, differential Doppler and modulation phase delay made using the CRABEX system on-board the Indian geostationary satellite GSAT2. The study shows that the PEC varies over a range of 10–22% (of the total electron content (TEC)) during daytime of magnetically quiet period. There is an increase in PEC with latitude during magnetically quiet period. During a magnetically disturbed period of 9 November 2004, the PEC increased to ∼30% of the TEC over the magnetic equatorial location of Trivandrum (8.5°N, 76.9°E, dip 0.5°N), while at Bangalore (13°N, 78°E, dip 10°N) it showed a large depletion. The implications of the new observations are discussed.     

Worst-Case GPS Scintillations on the Ground Estimated from Radio Occultation Observations of FORMOSAT-3/COSMIC During 2007–2014

The FORMOSAT-3/COSMIC (F3/C) satellite probes the S4 scintillation index profile of GPS signals by using the radio occultation (RO) technique. In this study, for practical use on the Earth’s surface, a method is developed to convert and integrate the probed RO S4 index, so obtaining the scintillation on the ground. To estimate the worst case, the maximum value on each profile probed by F3/C, which is termed S4max, is isolated. The isolated data are further used to construct the global three-dimensional distributions of S4max for various local times, seasons, solar activities, and locations. The converted S4max for the first time estimates the global distribution of ionospheric scintillations in the GPS L1 band C/A code signal on the ground. The results show that the worst-case scintillations appear within the low-latitude region of ±30°N, peaking around ±20°N magnetic latitude; they begin at 1900 MLT, reach their maximum at 2100 MLT, and vanish by about 0200–0300 MLT. The most pronounced low-latitude scintillation occurs over the South American and African sectors.     

Longitudinal variations in the daytime low-latitude ionosphere according to the data of topside sounding from the intercosmos-19 satellite

Using the data of the topside ionosphere sounding from the Intercosmos-19 satellite, longitudinal variations in foF2 at low latitudes at the daytime hours are considered. It is obtained that these variations in particular days in the majority of cases have a regular wave-like character with periods of about 75°–100° in longitude and amplitudes on the average of 2–4 MHz. In other words, along the valley and crests of the equatorial anomaly, a structure with four maximums and four minimums which have a tendency to be located near certain longitudes (the same in all seasons) is observed. The variations in foF2 along the crests of the equatorial anomaly are usually in anti-phase to variations along its valley. Comparing the characteristics of this wavelike structure at the daytime and nighttime hours, we obtained that the average positions of its extremes at the nighttime hours are shifted eastwards by 10°–50° relative to the daytime extremes. As a cause of formation of such a structure, high harmonics of atmospheric tides are assumed which, uplifting from below to heights of the E region, via the electric currents in this region influence the longitudinal structure of the electrodynamic plasma drift over the equator and by that impact the structure of the entire daytime low-latitude ionosphere.     

极点热层密度变化特征及其受太阳风扇形结构调制

本文基于2002年至2010年的GRACE卫星的观测密度统计分析南北极点的热层大气密度的世界时（即磁地方时）变化.研究发现：在9—11月份地球处于行星际磁场为背向太阳的扇区内（背向扇区）时,南极点热层密度在约17∶00 UT（13∶30 MLT）达到最大值,比日平均值高约22%;而在6—8月份,当地球处于行星际磁场为面向太阳的扇区内（面向扇区）时,北极点热层密度在06∶00 UT（12∶30 MLT）达到最大值,比日平均值高约13%.南极点的磁纬是-74°,其在15∶30 UT处于磁地方时正午,恰与极尖区位置重合.北极点在5∶30 UT处于磁地方时正午,此时北极点与极尖区位置最靠近.因此,极点热层大气密度的磁地方时变化可能是其周期性靠近极尖区的结果.南北极点热层密度的磁地方时变化分别在背向和面向扇区内更明显,这可能与行星际磁场B_y分量对南北半球密度的不同影响有关.统计结果还表明,极点热层大气密度的磁地方时变化在冬季半球内不明显.这可能是由于在冬季半球,沉降于极尖区的粒子相比夏季半球少、沉降高度低,因而能量沉降所引起的热层上部的密度增强较小.     

A statistical analysis of longitudinal dependences of upper thermospheric zonal winds at dip equator latitudes derived from CHAMP

New observations, obtained by the accelerometer onboard the CHAMP satellite, reveal a detailed picture of the thermospheric zonal wind. Based on three years of data (2002–2004) we have studied the longitudinal dependence of the zonal delta wind (deviations from the zonal average) at the dip equator. The large number of passes ($\sim$33 750) allows to consider several aspects of the wind characteristics at the same time. For this analysis we derived the longitudinal variation of the zonal delta wind at about 400 km altitude and investigated its dependence on solar flux, magnetic activity, and season. Major longitudinal dependences are confined to the morning hours, 03-09 local time (LT). The amplitude of the delta wind is approximately proportional to the latitudinal displacement of the magnetic dip equator from the geographic equator. The direction of the delta wind reverses sign between the June and December Solstices. During Equinox seasons these large scale features are almost absent. The flux level of solar EUV has no significant influence on the longitudinal variations. A dependence on magnetic activity could only be found during the post-sunset hours, 18-21 LT. Performing a Fourier transform of our delta wind velocities revealed a dominance of the wavenumber 4 in the Equinox data at some LT sectors. The wave-4 structure is a prevailing feature in the slowly precessing satellite frame, which has been recently reported, e.g. in nonmigrating tidal temperature measurements of the SABER instrument on the TIMED satellite in the Mesosphere Lower Thermosphere (MLT) region. Therefore, this statistical study of zonal wind longitudinal dependences provides new observational evidence for the coupling of the various atmospheric layers by nonmigrating tides.     

Morphology and causes of the Weddell Sea anomaly

The zone of anomalous diurnal variations in foF2, which is characterized by an excess of nighttime foF2 values over daytime ones, has been distinguished in the Southern Hemisphere based on the Intercosmos-19 satellite data. In English literature, this zone is usually defined as the Weddell Sea anomaly (WSA). The anomaly occupies the longitudes of 180°–360° E in the Western Hemisphere and the latitudes of 40°–80° S, and the effect is maximal (up to ∼5 MHz) at longitudes of 255°–315° E and latitudes of 60°–70° S (50°–55° ILAT). The anomaly is observed at all levels of solar activity. The anomaly formation causes have been considered based on calculations and qualitative analysis. For this purpose, the longitudinal variations in the ionospheric and thermospheric parameters in the Southern Hemisphere have been analyzed in detail for near-noon and near-midnight conditions. The analysis shows that the daytime foF2 values are much smaller in the Western Hemisphere than in the Eastern one, and, on the contrary, the nighttime values are much larger, as a result of which the foF2 diurnal variations are anomalous. Such a character of the longitudinal effect mainly depends on the vertical plasma drift under the action of the neutral wind and ionization by solar radiation. Other causes have also been considered: the composition and temperature of the atmosphere, plasma flows from the plasmasphere, electric fields, particle precipitation, and the relationship to the equatorial anomaly and the main ionospheric trough.     

Effects of neutral wind on the electron temperature at a height of 600 km in the low latitude region

Electron temperature observed by the Hinotori satellite with the low inclination at the height of \sim600 km was studied in terms of local time, season, latitude, magnetic declination and solar flux intensity during a 16-month period from 1981 to 1982. The electron temperatures show steep rise in the early morning (well known as morning overshoot), decrease after that and again increase at \sim18 hours (hereafter named as evening overshoot). Generally the morning overshoot becomes more enhanced in the winter hemisphere and for higher solar fluxes. The evening overshoot becomes more pronounced in the mid-latitude in all seasons and more enhanced in the winter hemisphere in the same way as the morning overshoot. A difference is seen between 210°-285° and 285°-360° longitudes where magnetic declination is different. The longitudinal dependence of electron temperature indicates that the neutral wind also contributes to the thermal structure in the low latitude ionosphere.     

Regional response of the mesosphere–lower thermosphere dynamics over Scandinavia to solar proton events and geomagnetic storms in late October 2003

The short-term regional responses of the mesosphere–lower thermosphere (MLT) dynamics over Scandinavia to the exceptionally strong solar storms with their accompanying solar proton fluxes on the Earth in late October 2003 have been investigated using radar measurements at Andenes (69°N, 16°E) and Esrange (68°N, 21°E). Several solar activity storms resulted in solar proton events (SPEs) at this time, but a particularly active period of high proton fluxes occurred between 28 and 31 October 2003. The significant temperature drop (∼25 K), detected by the meteor radar at Andenes at altitude ∼90 km, was in line with the enhancement of the proton fluxes and was caused by the dramatic reduction of the ozone in the high-latitude middle atmosphere monitored by satellite measurements. This exceptionally strong phenomenon in late October 2003 was composed of three geomagnetic storms, with the first one occurring in the daytime of 29 October and the other two storms in the nighttime of 29 and 30 October, respectively. The responses of the prevailing wind and the main tides (24- and 12-h tides) were studied in detail. It was found that the response of the MLT dynamics to the first geomagnetic storm occurring in the daytime and accompanied by solar proton fluxes is very different from those to the second and third geomagnetic storms with onsets during the nighttime. Some physical mechanisms have been suggested in order to explain the observed short-term variability of the MLT dynamics. This case study revealed the impact of the SPEs observed in late October 2003 and the timing of the geomagnetic storms on the MLT neutral wind responses observed over Scandinavia.     

Observations of 7-d planetary waves with MLT radars and the UARS-HRDI instrument

Long period variations in the mesosphere wind have been observed for some time by ground-based radars. These planetary scale disturbances have reoccurring periods at or near 5–7, 10, and 16 days and at times dominate the wind field at mesospheric heights. Recently, due to the continuous operation of several of the MLT radars and the availability of measurements from the UARS satellite, it has been possible to compare observations during periods of large planetary wave activity. Wind measurements from four MLT radars; the meteor radars at Durham, NH (43°N,71°W) and Sheffield, UK (53°N,2°W) and MF radars at Urbana, IL (40°N,88°W) and Saskatoon, Canada (52°N,107°W) were compared with the HRDI measurements during intervals when 7-d planetary waves were present. Wind data from the HRDI instrument on UARS has been processed to show the latitudinal structure and the seasonal variation of the planetary scale wind variation. The phases and amplitudes of the waves as determined by both the satellite and the radars are in good agreement. The ground-based measurements show large modulation of tides by these long period components, and also show comparable responses of these low frequency components over thousands of kilometers. The satellite and the ground-based results both indicate a preponderance of wave occurrence during the equinoxes and at preferred latitudes.     

Longitudinal variations in the hydroxyl emission: 1. Temperature

Data on longitudinal variations in the hydroxyl emission have been obtained based on long-term studies of the mesopause temperature and hydroxyl (OH) emission at different ground stations in the Northern Hemisphere and based on temperature measurements on the UARS WINDII satellite. Maximums at longitudes of Eurasia and North America and minimums over the Pacific and Atlantic oceans have been revealed in the global longitudinal temperature distribution. The average longitudinal temperature values show distinct seasonal variations. Local nonstationary large-scale inhomogeneities in the form of temperature maximums and minimums up to 30 K relative to the average temperature, correlating with the variations in the irregularity dimensions reaching several tens of degrees in longitude and latitude (which corresponds to several thousand kilometers), exist against a background of the average global temperature variation, reflecting the surface topography.