北京地区Pi2脉动和地磁AE指数的关系

分析了北京地区1998年1月1日至3月26日和4月24日至6月13日共136天记录的Pi2脉动事件特性,并与同时期亚暴AE指数进行了对比.结果发现,在北京地区越靠近日侧,观测到的Pi2脉动事件越少,幅度也越小.并不是每次亚暴都能激发空腔振荡模,亚暴强度的增加也并不代表空腔振荡模产生概率的增加.随着亚暴AE指数的增大,Pi2脉动的平均幅度基本上也在增大.但也有例外,可能是由于北京观测地点距离亚暴电流楔位置较远造成的.北京地区的Pi2脉动可以发生于亚暴的整个过程中,从AE指数开始增长期间（亚暴增长相）,一直到亚暴AE指数恢复正常（亚暴膨胀相后期）.某些亚暴没有对应着Pi2脉动事件,其AE指数从小于200nT一直到800nT以上.从观测数据来看,北京地区虽然纬度分区在低纬区域,但其Pi2脉动的特性与中纬Pi2特性更为靠近.所以不宜用北京地区Pi2来预报亚暴,以避免误报和漏报.     

低纬Pi2地磁脉动的多台观测

本文分析了1988年12月和1989年1月在长春、北京、兰州3个台站上观测的地磁脉动资料,研究了3个台站同时记录到的Pi2地磁脉动的频谱特征和偏振特性,进而对低纬Pi2地磁脉动的产生和传播机制做了理论研究.     

中低纬地区地磁脉动的研究

近年来我们对中低纬地区地磁脉动进行了大量的观测和研究。本文不仅介绍了观测仪器的设计、台网设置及数据处理方法。而且还简要地介绍了一些主要科研成果,如低纬Pc3脉动特点,低纬Pi2脉动偏振特性。南极地区的地磁脉动观测结果,以及在磁暴和太阳耀斑期间在低纬地区观测的地磁脉动。这对于进一步认识中低纬地区地磁脉动是十分有益的。     

Pi2地磁脉动的理论进展

目前，国内外在Ｐｉ２脉动的理论研究上取得了很大进展，现在问题的焦点是如何完整地解释Ｐｉ２脉动的全球特征和激发机制。解释Ｐｉ２脉动的理论主要有三种，即瞬态响应机制，亚暴电流楔理论和磁层空腔振荡理论。本文介绍了这三种理论的由来和发展，分析了每种理论在Ｐｉ２脉动研究中的贡献，并对Ｐｉ２脉动理论研究的进一步发展提出一些看法。     

利用地磁脉动预报地球同步轨道相对论电子通量的方法研究

本文利用低纬地磁台站的Pi1、Pi2地磁脉动（Pi1-2）资料和地球同步轨道的Pc5地磁脉动资料,对2004年1月到2006年12月38个磁暴事件的地磁脉动参数进行了统计分析.在此基础上,考虑相对论电子的局部加速机制,并加入损失机制,建立了一个初步的磁暴期间地球同步轨道相对论电子通量对数值的预报模型.利用该模型,我们对上述38个磁暴事件进行预报试验,最优化结果是：相对论电子通量对数值的预测值和观测值之间的线性相关系数为0.82,预报效率为0.67.这说明该模式具有较好的预报效果,也表明利用地磁脉动参数进行相对论电子通量预报是可行的.     

低纬Pc3脉动空间传播特性的研究

本文分析了从地球弓激波前的低纬磁流体波到低纬地面台站观测到Ｐｃ３脉动的整个传播过程,总结了国内外对低纬Ｐｃ３脉动传播特性在观测和理论上的主要研究成果,并对今后研究提出一些看法。     

亚暴期间高纬黄昏-子夜扇区极光弧增亮与衰减及其与IMF的关系

利用南极中山站极光全天空摄相、地磁、地磁脉动数据和Wind卫星的行星际磁场IMF观测数据，分析了7个亚暴期间高纬黄昏-子夜扇区极光弧的短暂增亮现象.极光弧特征是，短暂增亮随后很快衰减，历时10-20min，基本沿着日-地方向，有明显黄昏方向运动.这些事件大都发生在IMFB_z南转之后，亚暴增长相或膨胀相期间，极光浪涌到达之前10-73min消失.相应的IMFB_x＞0，IMFB_y＜0.这种极光弧和亚暴极光不同，它们与地磁活动及Pi2脉动不相关.这7个极光弧的形态和IMF特征表明，极光弧的增亮很可能由尾瓣重联产生，很快衰减归因于IMFB_z南向条件，而黄昏方向运动受IMFB_y控制.     

2005年8月24日磁暴主相期间亚暴过程的多卫星联合观测分析

本文根据OMNI、TC-2卫星、LANL系列卫星、Cluster星簇卫星(C1-C4)以及加拿大的8个中高纬地磁台站的观测数据,研究了2005年8月24日强磁暴(SYM-H_min~ -179 nT)主相期间的强亚暴(AL_min~ -4046 nT)事件特征.该强磁暴在大振幅(IMF B_{z min}~ -55.57 nT)、短持续时间(~90 min)的行星际磁场条件下产生,有明显的磁暴急始(SSC),强度较大且持续时间较短.发生在磁暴主相期间的亚暴发展的主要特征如下:亚暴增长相期间,C1-C4卫星先后穿越中心等离子体片;亚暴膨胀相触发后,在近地磁尾(X~-6R_E)可观测到磁场偶极化现象;等离子体无色散注入区在亚暴onset开始后迅速沿经向扩展,但被限制在有限的经度范围;磁纬60°附近,Pi2地磁脉动振幅超过了100 nT.膨胀相开始后,在中、高磁纬地磁台站可观测到负湾扰,近地磁尾可观测到Pi2空间脉动,中磁尾区域可观测到尾向流、磁重联以及O⁺/H⁺数密度比值在亚暴onset之后增大等现象.分析表明该强磁暴主相期间的强亚暴现象发生时序是自内向外:X~-6R_E处TC-2观测到磁场偶极化(~09:42:30 UT),同步轨道卫星LANL1994-084观测到等离子体无色散注入(~09:44:30 UT),X~-17.8R_E处C1观测到磁场重联(~09:45:30 UT),由此推断该亚暴事件很可能是近地磁尾不稳定性触发产生,其发生区域距离地球很近.     

极隙区Pc 3脉动特性的短基线研究

南极中山站和戴维斯站(不变磁纬74.5°)白天中午位于磁层极隙区,两站均安装了完全相同的感应式磁力计,选择1997年3月和1996年6、9、12月两站的数据,运用快速傅里叶变换和波形检查方法选择Pc3脉动事件,然后用信号互谱技术进行统计分析.结果如下:在中山站-戴维斯站,Pc3脉动主要出现于白天,尤其是中午/磁中午附近;Pc3脉动振幅及发生率均在6月份最小,在其他月份大些;Pc3脉动传播方向,白天主要向西.这些可能反映了电离层电导率和日侧电离层电流系统对Pc3脉动的影响.     

1998年8月6日亚暴期间极光电集流指数AE的特征分析

极光电集流指数(AE)被广泛用来定量描述由电离层电流引起的极光带地磁活动.AE指数也是宏观描述亚暴事件强度和发展过程的一个主要指标,它的优点在于简单直观和快速.本文对1998年8月6日系列亚暴事件的极光活动、电流体系和AE指数的形态特征进行了分析.结果表明,伪亚暴期间虽然AE指数大于500 nT 且有快速增长和缓慢恢复的形态,但是极光没有明显的极向或者赤道向的扩展,极区电流体系主要呈现对流特征;伪亚暴和亚暴期间AE指数的形态变化没有本质区别,但电集流中心的位置有很大差异.我们进一步分析了台站分布对AE指数计算的影响,探讨了伪亚暴和亚暴期间磁场扰动最大值所处的磁地方时的差异.     

First 10 min intervals of Pi2 onset at geosynchronous altitudes during the expansion of energetic ion regions in the nighttime sector

We examined the temporal variations of the geomagnetic field and energetic ions at geosynchronous altitudes associated with substorms during the nighttime using a superposed epoch analysis timed by Pi2 onset. We focused on the first 10 min intervals of Pi2 onset and on subsequent intervals to study the substorm expansion. We conclude that the first 10 min interval of Pi2 onset is a transitional state of the substorm dominated by MHD processes associated with earthward flow and its bifurcation. Intervals of field line variations following the first 10 min were well organized by dipolarization (substorm current wedge) due to the reduced cross-tail current. We also show that energetic ion regions localized in the local time sector from 2000 to 0000 LT in the first 10 min intervals of Pi2 onset expanded to the post-midnight sector, reaching 0400 LT within 20 min after Pi2 onset. We conclude that the expansion of the energetic plasma regions can be attributed to the inflation of the inner magnetosphere during dipolarization.     

SABRE observations of Pi2 pulsations: case studies

The characteristics of substorm-associated Pi2 pulsations observed by the SABRE coherent radar system during three separate case studies are presented. The SABRE field of view is well positioned to observe the differences between the auroral zone pulsation signature and that observed at mid-latitudes. During the first case study the SABRE field of view is initially in the eastward electrojet, equatorward and to the west of the substorm-enhanced electrojet current. As the interval progresses, the western, upward field-aligned current of the substorm current wedge moves westward across the longitudes of the radar field of view. The westward motion of the wedge is apparent in the spatial and temporal signatures of the associated Pi2 pulsation spectra and polarisation sense. During the second case study, the complex field-aligned and ionospheric currents associated with the pulsation generation region move equatorward into the SABRE field of view and then poleward out of it again after the third pulsation in the series. The spectral content of the four pulsations during the interval indicate different auroral zone and mid-latitude signatures. The final case study is from a period of low magnetic activity when SABRE observes a Pi2 pulsation signature from regions equatorward of the enhanced substorm currents. There is an apparent mode change between the signature observed by SABRE in the ionosphere and that on the ground by magnetometers at latitudes slightly equatorward of the radar field of view. The observations are discussed in terms of published theories of the generation mechanisms for this type of pulsation. Different signatures are observed by SABRE depending on the level of magnetic activity and the position of the SABRE field of view relative to the pulsation generation region. A twin source model for Pi2 pulsation generation provides the clearest explanation of the signatures observed.     

SABRE observations of structured ionospheric flows during substorm expansion phase onset

The irregularity velocity patterns observed by the SABRE coherent radar at substorm expansion phase onset, which is identified by magnetometer observations of Pi2 pulsations, are occasionally highly structured. In all the examples of structured velocity patterns examined, the SABRE viewing area is located at longitudes within the inferred substorm current wedge. Three types of structured velocity regime are apparent depending on the level of magnetic activity and the position of the radar viewing area relative to the substorm enhanced currents and the Pi2 pulsation generation region. Firstly, vortex-like velocity patterns are observed and these may be caused by the field-aligned currents associated with the substorm current wedge. Secondly, regions of equatorward velocity are also observed at times of substorm expansion phase onset moving longitudinally across the SABRE viewing area. The longitudinal movement is usually westward although an example of eastward motion has been observed. The phase velocity of these regions of equatorward flow is typically 1–3 km s^?1. The observed equatorward velocities occur at the poleward edge or poleward of the background convection velocities observed by SABRE. These equatorward velocities may be related to the westward travelling surge and to the expansion (eastwards as well as westwards) of the brightening arc region at substorm onset. Thirdly, the flow rotates equatorward within the field of view but does not then appear to move longitudinally. These equatorward velocities may relate to the earthward surge of plasma from the magnetotail at substorm onset.     

Multipoint observations of Pi2 pulsations and correlation with dynamic processes in the near-Earth magnetotail on March 18, 2009

Simultaneous measurements from THEMIS spacecraft,GOES-11 and ground stations(Canadian Array for Realtime Investigations of Magnetic Activity or CARISMA,and 210°magnetic meridian or MM)on March 18,2009 allow the study of dynamic processes in the near-Earth magnetotail and corresponding Pi2 pulsations on the ground in great detail.Fast earthward flows along with traveling Alfvén waves and fast mode waves in the Pi2 band were observed by three Time History of Events and Macroscale Interactions during Substorms(THEMIS)probes(P3,P4 and P5)in the near-Earth plasmasheet.At the mid-to high-latitude nightside,the CARISMA stations located near the foot points of the three probes recorded Pi2s with two periods,about 80 s after the earthward fast flows observed by the P4 probe.The long-period Pi2(140–150 s)belongs to the transient response Pi2(TR Pi2),since the travel time of the Alfvén waves between the plasma sheet and CARISMA stations is very close to half the period of the long-period Pi2.The short-period Pi2(60–80 s)has the same period band as the perpendicular velocity of the fast flows,which indicates that it may relate to the inertial current caused by periodic braking of the earthward fast flows.The 210°MM stations located at the low-latitude duskside also observed Pi2s with the same start time,waveform and frequency,about~120 s after the earthward fast flows.Strong poloidal oscillations are shown by GOES-11(~23 MLT)and the compressional component(Bb)is highly correlated with H components of the 210°MM stations,whereas the other two components(Br and Be)are not.These results confirm that the low-latitude Pi2s are generated by cavity mode resonance,which is driven by an impulsive broadband source in the near-Earth magnetotail.     

Decay of the Dst field of geomagnetic disturbance after substorm onset and its implication to storm-substorm relation

In order to investigate the causal relationship between magnetic storms and substorms, variations of the mid-latitude geomagnetic indices, ASY (asymmetric part) and SYM (symmetric part), at substorm onsets are examined. Substorm onsets are defined by three different phenomena; (1) a rapid increase in the mid-latitude asymmetric-disturbance indices, ASY-D and ASY-H, with a shape of so-called ‘mid-latitude positive bay’; (2) a sharp decrease in the AL index; (3) an onset of Pi2 geomagnetic pulsation. The positive bays are selected using eye inspection and a pattern-matching technique. The 1-min-resolution SYM-H index, which is essentially the same as the hourly Dst index except in terms of the time resolution, does not show any statistically significant development after the onset of substorms; it tends to decay after the onset rather than to develop. It is suggested by a simple model calculation that the decay of the magnetospheric tail current after substorm onset is responsible for the decay of the Dst field. The relation between the IMF southward turning and the development of the Dst field is reexamined. The results support the idea that the geomagnetic storms and substorms are independent processes; that is, the ring-current development is not the result of the frequent occurrence of substorms, but that of enhanced convection caused by the large southward IMF. A substorm is the process of energy dissipation in the magnetosphere, and its contribution to the storm-time ring-current formation seems to be negligible. The decay of the Dst field after a substorm onset is explained by a magnetospheric energy theorem.     

一种基于紫外极光图像的亚暴膨胀期起始时刻的自动检测方法

准确界定亚暴起始时刻是理解亚暴相关问题的关键.已有研究主要集中在两方面:一是从极光图像中人工挑选亚暴事件进行案例分析或统计分析来研究亚暴发生机制及亚暴期间的地磁环境;二是基于一些空间物理参数,如AE指数、SME(SuperMAG electrojet)指数、Pi2、正弯扰等,采用人眼判断或是模式识别的方法从中找出亚暴起始时刻.本文尝试采用模式识别的方法从紫外极光图像中自动地检测出亚暴膨胀期起始时刻.首先,将紫外极光图像通过网格化处理转换到磁地方时-地磁纬度(MLT-MLAT)直角坐标下,然后通过模糊c均值聚类方法提取亮斑,再考察亮斑强度是否增强、面积是否极向膨胀来判断是不是亚暴事件.本文方法在1996年12月-1997年2月这三个月的Polar卫星紫外极光图像上进行了实验验证.我们将检测到的亚暴起始时刻与Liou(J. Geophys. Res., 2010, 115: A12219)的人工标记进行了对比,并详细分析了与标记不一致的多检和漏检事件.本文提出的自动检测方法可以快速地从海量紫外极光图像中完成亚暴事件的初步筛选,方便研究人员进一步深入研究极光亚暴.     

Substorm onset identification using neural networks and Pi2 pulsations

The pattern recognition capabilities of artificial neural networks (ANNs) have for the first time been used to identify Pi2 pulsations in magnetometer data, which in turn serve as indicators of substorm onsets and intensifications. The pulsation spectrum was used as input to the ANN and the network was trained to give an output of +1 for Pi2 signatures and –1 for non-Pi2 signatures. In order to evaluate the degree of success of the neural-network procedure for identifying Pi2 pulsations, the ANN was used to scan a number of data sets and the results compared with visual identification of Pi2 signatures. The ANN performed extremely well with a success rate of approximately 90% for Pi2 identification and a timing accuracy generally within 1 min compared to visual identification. A number of potential applications of the neural-network Pi2 scanning procedure are discussed.