The high latitude convection response to an interval of substorm activity

On 17 March 1991, five clear substorm onsets/intensifications took place within a three hour interval. During this interval ground-based data from the EISCAT incoherent scatter radar, a digital CCD all sky camera, and an extensive array of magnetometers were available, in addition to data from the CRRES and DMSP spacecraft, whose footprints passed over Scandinavia very close to most of the ground-based instrumentation. This interval of substorm activity has been interpreted as being in support of a near-Earth current disruption model of substorm onset. In the present study the ionospheric convection response, observed some four hours to the west in MLT by the Halley HF radar in Antarctica, is related to the growth, expansion and recovery phases of two of the substorm onsets/expansions observed in the Northern Hemisphere. Bursts of ionospheric flow and motion of the convection reversal boundary (CRB) are observed at Halley in response to the substorm activity and changes in the IMF. The delay between the substorm expansion phase onset and the response in the CRB location is dependent on the local time separation from, and latitude of, the initial substorm onset region. These results are interpreted in terms of a synthesis of the very near-Earth current disruption model and the near-Earth neutral line model of substorm onset.     

Interhemispheric contrasts in the ionospheric convection response to changes in the interplanetary magnetic field and substorm activity: a case-study

Interhemispheric contrasts in the ionospheric convection response to variations of the interplanetary magnetic field (IMF) and substorm activity are examined, for an interval observed by the Polar Anglo-American Conjugate Experiment (PACE) radar system between 1600 and 2100 MLT on 4 March 1992. Representations of the ionospheric convection pattern associated with different orientations and magnitudes of the IMF and nightside driven enhancements of the auroral electrojet are employed to illustrate a possible explanation for the contrast in convection flow response observed in radar data at nominally conjugate points. Ion drift measurements from the Defence Meteorological Satellite Program (DMSP) confirm these ionospheric convection flows to be representative for the prevailing IMF orientation and magnitude. The location of the fields of view of the PACE radars with respect to these patterns suggest that the radar backscatter observed in each hemisphere is critically influenced by the position of the ionospheric convection reversal boundary (CRB) within the radar field of view and the influence it has on the generation of the irregularities required as scattering targets by high-frequency coherent radar systems. The position of the CRB in each hemisphere is strongly controlled by the relative magnitudes of the IMF B_z and B_y components, and hence so is the interhemispheric contrast in the radar observations.     

Variations in the polar cap area during intervals of substorm activity on 20–21 March 1990 deduced from AMIE convection patterns

The dynamic behaviour of the northern polar cap area is studied employing Northern Hemisphere electric potential patterns derived by the Assimilative Mapping of Ionospheric Electrodynamics (AMIE) procedure. The rate of change in area of the polar cap, which can be defined as the region of magnetospheric field lines open to the interplanetary magnetic field (IMF), has been calculated during two intervals when the IMF had an approximately constant southward component (1100- 2200 UT, 20 March 1990 and 1300–2100 UT, 21 March 1990). The estimates of the polar cap area are based on the approximation of the polar cap boundary by the flow reversal boundary. The change in the polar cap area is then compared to the predicted expansion rate based on a simple application of Faraday’s Law. Furthermore, timings of magnetospheric substorms are also related to changes in the polar cap area. Once the convection electric field reconfigures following a southward turning of the IMF, the growth rate of the observed polar cap boundary is consistent with that predicted by Faraday’s Law. A delay of typically 20 min to 50 min is observed between a substorm expansion phase onset and a reduction in the polar cap area. Such a delay is consistent with a synthesis between the near Earth neutral line and current disruption models of magnetospheric substorms in which the dipolarisation in the magnetotail may act as a trigger for reconnection. These delays may represent a propagation time between near geosynchronous orbit dipolarisation and subsequent reconnection further down tail. We estimate, from these delays, that the neutral X line occurs between \sim35R_E and \sim75R_E downstream in the tail.     

Central polar cap convection response to short duration southward Interplanetary Magnetic Field

Central polar cap convection changes associated with southward turnings of the Interplanetary Magnetic Field (IMF) are studied using a chain of Canadian Advanced Digital Ionosondes (CADI) in the northern polar cap. A study of 32 short duration (1 h) southward IMF transition events found a three stage response: (1) initial response to a southward transition is near simultaneous for the entire polar cap; (2) the peak of the convection speed (attributed to the maximum merging electric field) propagates poleward from the ionospheric footprint of the merging region; and (3) if the change in IMF is rapid enough, then a step in convection appears to start at the cusp and then propagates antisunward over the polar cap with the velocity of the maximum convection. On the nightside, a substorm onset is observed at about the time when the step increase in convection (associated with the rapid transition of IMF) arrives at the polar cap boundary.     

Extended period of polar cap auroral display: auroral dynamics and relation to the IMF and the ionospheric convection

An unusually extended period (5 h) of polar cap auroral display on 3 August 1986 is examined. Auroras have been investigated using ground-based data as well as measurements from the IMP-8 spacecraft in interplanetary space and simultaneous observations from the polar-orbiting satellites Viking and DE-1 in the northern and southern hemispheres, respectively. It is found that visible Sun-aligned arcs are located inside the transpolar band of the -aurora observed from the satellite in ultraviolet wavelengths. The transpolar band can contain several Sun-aligned arcs that move inside the band toward the morning or evening side of the auroral oval independent of the direction of the band movement. Intensifications of polar cap auroras with durations of up to about 30 min are observed. No change has been found in either IMF parameters or substorm activity that can be related to these intensifications. The -aurora occurred during a 2-h period when the B _z-component of the IMF was negative. A tendency is noted for dawnward (duskward) displacement of the transpolar band when B_y>0 (B_y<0) in the southern hemisphere. Simultaneous observations of auroral ovals during interplanetary B_z<0, B_y<0 and B_x>0 in both hemispheres and convection patterns for B_z<0 and B_y<0 have been displayed using satellite and ground-based measurements. It was found that the transpolar band of the -aurora in the sunlit hemisphere was situated in the region of large-scale downward Birkeland currents.     

对流输运在TOI断裂形成等离子体云块中的作用研究

极盖等离子体云块是极区电离层常见特征之一,其形成演化过程是当前重要研究课题.光电离高密度等离子体在对流输送作用下从日侧穿过极隙,通过极盖到达夜侧,已成为共识.日侧磁场重联作用下的极区对流输运过程,在舌状等离子体结构（TOI）"断裂"形成极盖等离子体云块中发挥重要作用.利用极区全域GPS/TEC观测数据,结合SuperDARN雷达实测的对流速度,对等离子体云块形成过程进行案例研究,重点分析两种TOI断裂形成等离子体云块的发生机制.研究结果显示,等离子体对流输运过程在TOI断裂形成等离子体云块过程中发挥关键性作用,对流形态或局部对流速度矢量急剧变化都可能导致TOI结构不稳定,使TOI结构断裂形成等离子体云块.     

对流输运在TOI断裂形成等离子体云块中的作用研究

极盖等离子体云块是极区电离层常见特征之一,其形成演化过程是当前重要研究课题.光电离高密度等离子体在对流输送作用下从日侧穿过极隙,通过极盖到达夜侧,已成为共识.日侧磁场重联作用下的极区对流输运过程,在舌状等离子体结构（TOI）"断裂"形成极盖等离子体云块中发挥重要作用.利用极区全域GPS/TEC观测数据,结合SuperDARN雷达实测的对流速度,对等离子体云块形成过程进行案例研究,重点分析两种TOI断裂形成等离子体云块的发生机制.研究结果显示,等离子体对流输运过程在TOI断裂形成等离子体云块过程中发挥关键性作用,对流形态或局部对流速度矢量急剧变化都可能导致TOI结构不稳定,使TOI结构断裂形成等离子体云块.     

极区电离层对流速度的浅层神经网络建模与分析

电离层对流是太阳风与地球磁场相互作用下驱动的磁层大尺度对流循环与对流电场在极区电离层的映射, 与行星际磁场-地球磁场耦合系统息息相关.本文基于SuperDARN(Super Dual Aurora Radar Network)分布在北半球的23部高频相干散射雷达获取到的二维电离层对流速度对其进行建模研究.模型输入为行星际磁场三分量、太阳风速度、太阳风密度和地磁指数六个空间物理参数, 模型输出为二维对流速度.模型选择两种广泛应用于空间物理建模的浅层神经网络即广义回归神经网络(General Regression Neural Network, GRNN)和误差反向传播(Back Propagation, BP)神经网络.实验结果显示, GRNN模型和BP模型的速度幅值均方根误差分别为174.96 m·s^-1和234.21 m·s^-1, 速度方向角均方根误差分别达到62.30°和88.07°, 相比于对流速度最大值2000 m·s^-1和360°的方向角范围来说, 其误差是可以接受的.外推性实验结果显示, 在第24个太阳周期时, GRNN模型和BP模型的速度幅值均方根误差分别为305.35 m·s^-1和738.15 m·s^-1, 速度方向角均方根误差分别为82.01°和90.56°.实验结果表明, GRNN在时间外推性上的效果优于BP神经网络, 更适用于预测对流速度.我们发现在四种典型空间环境条件下, 利用GRNN模型预测的瞬时对流速度来构建的全域对流模式与现有统计模型构建的对流模式相似, 从而验证预测的对流速度可以用于分析瞬时极区电离层对流.

     

The convection electrojet and the substorm electrojet

Enhancements in the auroral electrojets associated with magnetospheric substorms result from those in either the electric field or the ionospheric conductivities, or both. Their relative importance varies significantly, even during a single substorm, depending on the location as well as on the substorm phases. It is predicted that different parts of the electrojets tend to respond in different ways to substorm activity. The unprecedented, unique opportunity for CLUSTER spacecraft observations of electric/magnetic fields and precipitating particles, combined with radar measurements of ionospheric quantities and with ground magnetometers, will provide us with crucial information regarding the physical nature of the separation between the “electric field-dominant” and “conductivity-dominant” auroral electrojets. This study also discusses the implications of these two auroral-electrojet components in terms of solar wind-magnetosphere-ionosphere interactions.     

基于深度学习的SuperDARN雷达极区电离层对流电势模型构建及预测

电离层等离子体对流是表征电离层电动力学的重要现象,对空间天气有着重要的指示作用.SuperDARN雷达网是研究中高纬电离层对流的重要手段,也是获得对流电势数据的重要来源.本文基于SuperDARN雷达12月份的对流电势数据,采用BP模型、FC-LSTM模型以及ED-ConvLSTM时空序列模型构建了高纬电离层等离子体对流电势30min预测模型,然后采用独立的数据集,基于预测值与实测值的结构相似度（SSIM）、均方根误差（RMSE）以及线性相关系数（LC）三个统计指标对模型的性能进行了评估,同时分析对比了三种模型预测的越极盖电势（CPCP）和越极盖电场（CPEF）与实测值的统计分布情况.结果表明,BP模型和FC-LSTM模型由于没有充分挖掘到空间上的信息,因此整体误差较大,前者SSIM、LC以及RMSE分别为0.80、0.89、4.38 kV,后者为0.76、0.86、4.96 kV,而ED-ConvLSTM模型则分别为0.83、0.91、3.96 kV,因其能充分捕捉到空间上的信息,三个指标明显优于前两种模型,同时在CPCP分布和CPEF分布的相似度上,ED-ConvLSTM模型性能也表现得最好.本文结果证明了时空序列模型ED-ConvLSTM在对流电势预测上的有效性.

     

Relationship between the ionospheric potential and the ground-level electric field in the southern polar cap

The relationships between the average hourly values of the vertical ground-level electric field measured at the Vostok Antarctic station and the ionospheric potential above the station have been obtained. The ΔEz and Uext parts of both parameters controlled by the solar wind were considered. Convection models (Weimer, 1995; Lukianova and Christiansen, 2006) and a model based on the SuperDARN radar system were used to determine the ionospheric potential. An analysis has been performed for isolated days and the entire sample in 1998–2000 (including 170 days of “fine weather”). For an isolated day, the best correlation coefficients (R) between ΔEz and Uext obtained using the three models were 0.81, 0.80, and 0.88, respectively. The total correlation coefficient for the entire data set was R = 0.24−0.32. The R value was larger during daytime (R ≈ 0.4) and smaller at night (R ≈ 0.1) and slightly increased in the early morning hours. The specific features of daily variations in R apparently indicate that it is possible to adequately describe the structure of the ionospheric electric field equipotentials by using large-scale stationary convection models. The R value varies complexly, depending on the IMF orientation, but it generally tends to increase from IMF By < 0 to By > 0, which is explained by the asymmetric convection patterns for opposite By signs.     

一次行星际磁场南向突变的高纬电离层对流响应特征

本文利用北半球的超级双极光雷达网数据,考察了一次行星际磁场南向突变时高纬电离层对流的响应特征,着重分析了响应的时间尺度. 对所研究的事件,行星际磁场南北分量在1.5 min内从+7 nT突变到-8 nT,而在突变前后约40 min内都保持相对稳定. 结果表明,电离层对流的初始响应发生在磁正午附近,相对于行星际磁场突变到达磁层顶的时间有大约3 min的滞后;响应与磁地方时有明显依赖关系,离磁正午越远,响应的滞后时间越长,晨昏两侧的对流响应比磁正午滞后约6 min,磁午夜的对流响应比磁正午滞后约12 min;对流重新趋于稳定的时间与磁地方时没有明显的依赖关系,该时间尺度约为10～14 min.     

SuperDARN studies of the ionospheric convection response to a northward turning of the interplanetary magnetic field

The response of the dayside ionospheric flow to a sharp change in the direction of the interplanetary magnetic field (IMF) measured by the WIND spacecraft from negative B_z and positive B_y, to positive B_z and small B_y, has been studied using SuperDARN radar, DMSP satellite, and ground magnetometer data. In response to the IMF change, the flow underwent a transition from a distorted twin-cell flow involving antisunward flow over the polar cap, to a multi-cell flow involving a region of sunward flow at high latitudes near noon. The radar data have been studied at the highest time resolution available (2 min) to determine how this transition took place. It is found that the dayside flow responded promptly to the change in the IMF, with changes in radar and magnetic data starting within a few minutes of the estimated time at which the effects could first have reached the dayside ionosphere. The data also indicate that sunward flows appeared promptly at the start of the flow change (within 2 min), localised initially in a small region near noon at the equatorward edge of the radar backscatter band. Subsequently the region occupied by these flows expanded rapidly east-west and poleward, over intervals of 7 and 14 min respectively, to cover a region at least 2 h wide in local time and 5° in latitude, before rapid evolution ceased in the noon sector. In the lower latitude dusk sector the evolution extended for a further 6 min before quasi-steady conditions again prevailed within the field-of-view. Overall, these observations are shown to be in close conformity with expectations based on prior theoretical discussion, except for the very prompt appearance of sunward flows after the onset of the flow change.     

Interhemispheric observations of nightside ionospheric electric fields in response to IMF B z and B y changes and substorm pseudobreakup

HF radar data during equinoctial, small IMF B_y conditions have enabled the ionospheric convection during the substorm growth phase and substorm pseudobreakup to be studied in both hemispheres. This has revealed both conjugate and non-conjugate convection behaviour during the substorm growth phase before and after the pseudobreakup onset. The nightside convection pattern is found to respond promptly to the southward turning of the interplanetary magnetic field (IMF) which impacts on the dusk flank of the magnetosphere due to an inclined phase front in the IMF in the case study presented. The subsequent interhemispheric observations of nightside convection are controlled by the IMF B_y polarity. The time scale for the response to changes in the IMF B_y component is found to be a little longer than for B_z, and the full impact of the IMF B_y is not apparent in the nightside convection until after substorm pseudobreakup has occurred. The pseudobreakup itself is found to result in a transitory suppression in the ionospheric electric field in both hemispheres. This flow suppression is very similar to that observed in HF radar observations of full substorm onset, with the exception of a lack of subsequent poleward expansion.     

The dawn and dusk electrojet response to substorm onset

We have investigated the time delay between substorm onset and related reactions in the dawn and dusk ionospheric electrojets, clearly separated from the nightside located substorm current wedge by several hours in MLT. We looked for substorm onsets occurring over Greenland, where the onset was identified by a LANL satellite and DMI magnetometers located on Greenland. With this setup the MARIA magnetometer network was located at dusk, monitoring the eastward electrojet, and the IMAGE chain at dawn, for the westward jet. In the first few minutes following substorm onset, sudden enhancements of the electrojets were identified by looking for rapid changes in magnetograms. These results show that the speed of information transfer between the region of onset and the dawn and dusk ionosphere is very high. A number of events where the reaction seemed to preceed the onset were explained by either unfavorable instrument locations, preventing proper onset timing, or by the inner magnetospheres reaction to the Earthward fast flows from the near-Earth neutral line model. Case studies with ionospheric coherent (SuperDARN) and incoherent (EISCAT) radars have been performed to see whether a convection-induced electric field or enhanced conductivity is the main agent for the reactions in the electrojets. The results indicate an imposed electric field enhancement.     

Relationship between magnetic activity in the polar cap and atmospheric processes in the winter Antarctica

The paper demonstrates the close relationships between the polar cap magnetic activity, which is characterized by PC index (Troshichev et al., 1988, Troshichev et al., 2006) and some atmospheric phenomena typical of the winter Antarctica, such as enhancement of cloudiness, sudden warmings of the ground atmosphere in near-pole area, and formation of anomalous wind regimes above Antarctica. It was shown previously (Troshichev et al., 2004, Troshichev et al., 2008, Troshichev and Janzhura, 2004) that these atmospheric phenomena are controlled by variations of the geoeffective interplanetary electric field impacting the Earth’s magnetosphere. On the other hand, the polar cap magnetic activity is also determined by the interplanetary electric field influence through the field-aligned magnetospheric currents and electric field in the polar cap ionosphere. The results imply that the PC index, available online at http://www.aari.nw.ru from the near-pole station Vostok, can be used to monitor the anomalous atmospheric processes in winter Antarctica.     

Letter to the editor The ionospheric response during an interval of Pc5 ULF wave activity

A preliminary analysis of Pc5, ULF wave activity observed with the IMAGE magnetometer array and the EISCAT UHF radar in the post midnight sector indicates that such waves can be caused by the modulation of the ionospheric conductivity as well as the wave electric field. An observed Pc5 pulsation is divided into three separate intervals based upon the EISCAT data. In the first and third, the Pc5 waves are observed only in the measured electron density between 90 and 112 km and maxima in the electron density at these altitudes are attributed to pulsed precipitation of electrons with energies up to 40 keV which result in the height integrated Hall conductivity being pulsed between 10 and 50 S. In the second interval, the Pc5 wave is observed in the F-region ion temperature, electron density and electron temperature but not in the D and E region electron densities. The analysis suggests that the wave during this interval is a coupled Alfven and compressional mode.