Variation of dependence of the cusp location at different altitude on the dipole tilt

Using the Cluster cusp crossings data, dependence of the cusp location at the mid-altitude on the geomagnetic dipole tilt during northward IMF is studied. The results show that the cusp center moves 0.051° Invariant Latitude (ILAT) upon the increase of 1° in the dipole tilt angle at the average altitude of 5.8 R_E (Earth radius). According to the present results obtained at the altitude of the Cluster orbit and previous results obtained at other altitudes of other satellite orbits, it is found that the higher the altitude in the cusp region is, the bigger the dependence of cusp location on the dipole tilt angle will be. If the altitude increases by 1 R_E in the cusp region, the dependence will increase by 0.012° ILAT upon the increase of 1° in the dipole tilt angle. Some possible physical mechanisms are discussed and it shows that the cusp location will be more sensitive to the solar wind dynamic pressure if the altitude is high.     

ACE飞船观测的行星际磁场准27天重现周期和结构

 ACE飞船发射于1997年8月15日,将维持到2024年,位于日地连线重力平衡点L1。本文采用ACE飞船行星际磁场观测数据,基于GSE坐标系统,确定L1点的行星际磁场主体方位,进而将行星际磁场观测数据转换为极性符号序列。对于序列中的任一时间点,通过改变以它为中心的子序列探测行星际磁场的准27d重现周期和结构,再应用模板匹配方法识别重现结构,最后采用分段常值函数拟合获得分段稳定的周期和结构。得到的主要结果如下：(1) 1999—2008年间,IMF重现周期绝大多数在(27±2)d范围内,只有1个例外,即2001年10月27日10:00—11月28日12:00时间内,重现周期为21d14h;(2) 2001年1月8日12:00—2004年7月17日04:00,IMF为2扇瓣结构,2004年7月17日05:00—2007年6月30日23:00,IMF为4扇瓣结构,2007年7月1日00:00—2008年12月31日23:00,IMF为2扇瓣结构。     

Field-aligned current distribution and response to interplanetary conditions during a superstorm―CHAMP observation

With geomagnetic measurements on board of CHAMP satellite, the characteristics of global large-scale field-aligned currents （FACs） in the topside ionosphere are investigated along with their responses to interplanetary conditions for the superstorm of November, 2003. It is found that （1） The storm-time FAC densities enhanced greatly in comparison with quiet period and the enhancements show hemispheric asymmetry of both summer-winter and sunlit-dark. （2） For the first time, it is revealed that the lati- tude-integrated FAC density is controlled mainly by solar wind dynamic pressure rather than iMF. （3） FACs expanded equatorward dramatically, with the lowest latitude being 45° MLat or more; on the dayside this expansion was controlled directly by IMF Bz, showing an interaction time scale of about 25 min in the solar wind-magnetosphere-ionosphere coupling system, and a nonlinear saturation of the equatorward expansion when IMF Bz 〈 -30 nT; while on the nightside, the expansion and recovery lagged about 3 h behind the IMF changes but nearly in phase with changes of SYM-H index. （4） During the storm main phase, the nightside FAC latitude coverage extended to 25° or wider, appearing multi-sheet current structure with more than 10 sheets.     

Magnetic Storm Effects in the Auroral Ionosphere Observed with EISCAT Radar -Two Case Studies

Storm-time changes of main plasma parameters in the auroral ionosphere are analyzed for two intense storms occurring on May 15, 1997 and Sept. 25, 1998, with emphasis on their relationship to the solar wind dynamic pressure and the IMF Bz component. Strong hard particle precipitation occurred in the initial phase for both storma,associated with high solar wind dynamical pressure. During the recovery phase of the storms, some strong particle precipitation was neither concerned with high solar wind pressure nor southward IMF Bz. Severe negative storm effects depicted by electron density depletion appeared in theF-region during the main and recovery phase of both storms, caused by intensive electric field-related strong Joule/frictional heating when IMF was largely southward. The ion temperature behaved similarly in E- and F-region, but the electron temperature did quite different, with a strong increase in the lower E-region relating to plasma instability excited by strong electric field and a slight decrease in the F-region probably concerning with a cooling process. The field-aligned ion velocity was high and apparently anticorrelated with the northward component of the ion convection velocity.     

覆盖层厚度对远场长周期地震动能量特性的影响研究

选取汶川8.0级地震中陕西省6个台站的东西向地震动加速度记录,通过HHT计算了各条地震动和其IMF分量的Hilbert能量和输入能量,对比分析了覆盖层厚度对远场长周期地震动能量特性的影响。结果表明：随着覆盖层厚度的增加,地震动的HE峰值、输入能量和Hilbert能量平均周期T_mE逐渐增加,当覆盖层厚度大于400m时,地震动能量主要分布在低频区域,具有显著的长周期特性;当覆盖层厚度为0或很小时,地震动能量主要集中在前2-3阶IMF分量中,多个IMF分量的HE峰值较大,卓越IMF分量对结构的影响较小;随着覆盖层厚度的增加,地震动能量主要集中在高阶IMF分量中,仅1-2个IMF分量的HE峰值较大,其余分量均很小,卓越IMF分量的平均周期T_mE和原始地震动十分接近,对结构的破坏起主导作用,应重点研究。     

Enhanced anti-sunward flow near local noon during a period of horizontal IMF and high solar wind velocity <Emphasis Type="Italic">V</Emphasis><Subscript><Emphasis Type="Italic">Y</Emphasis></Subscript>

It is believed that a southward interplanetary magnetic field (IMF) is mainly responsible for the energy input from solar wind into the magnetosphere. This paper presents an unusual case of strong anti-sunward plasma flow (up to 2 km/s) in the polar cap ionosphere and large cross-polar cap potential (CPCP) during a period of horizontal IMF (|B _Z | < 2 nT) observed by both ACE (at the L1 point) and Geotail (on the dusk flank of the magnetosheath). The CPCP is even higher than that under preceding B _Z ≈ −23 nT. Furthermore, GOES8 observed that the magnetosheath field turns northward as the anti-sunward plasma flow and CPCP start to increase, which implies that the magnetosheath field interacting with the Earth’s magnetopause has significantly rotated and differs from the IMF observed by ACE and Geotail. In accordance with previous theoretical work, we suggest that the magnetic field line draping produces a southward magnetosheath field and enhances anti-sunward plasma flow and the CPCP.     

Comparative study of a substorm event by satellite observation and model simulation

A substorm event has been simulated for the first time by using SWMF (Space Weather Modeling Framework) developed by the University of Michigan. The model results have been validated using Geotail and Cluster satellite observations. The substorm onset occurs at 22:08 UT on September 28, 2004, as identified from FUV WIC observations on the NASA IMAGE spacecraft. SWMF can couple effectively the magnetosphere, inner magnetosphere and ionosphere processes and is driven by the solar wind and IMF (Interplanetary Magnetic Field) parameters, which are measured by ACE satellite and time delayed to the upstream boundary of the model. It shows that (1) SWMF can predict well the large-scale variations of the magnetospheric magnetic field and ionospheric currents during the substorm event; and (2) the accuracy of the time delay of the solar wind from ACE to the outer boundary of the model has great effects on the model results. Finally, the substorm trigger mechanism has been discussed and the way of improvement of the model has been pointed out.     

基于希尔伯特-黄变换的径流规律分析

希尔伯特－黄变换在处理非线性、非平稳、弱相依、高度复杂的时间序列时,比传统的时间序列分析方法更具优势。通过对时间序列进行经验模态分解（EMD）,得到若干反映时间序列演化过程的本征模态函数（IMF）和序列变化的残余项（趋势项）,然后对每个本征模态函数作希尔伯特－黄变换,得到反映径流规律的统计特征值,从而获得序列变化的周期。对渭河临潼水文站的年径流观测数据进行分析,得出年径流变化存在9．52年、13．70年、21．74年和41．67年的周期,且有逐渐减小的趋势。     

A preliminary exploration of the mechanism for the occurrence of two types of various magnetic structures in the magnetotail

As well known, the magnetic cross-tail component B_y in the magnetotail is in direct proportion to the in-terplanetary magnetic field (IMF) B_y component. And the polarity of IMF and plasmoid / flux rope B_y components do indeed agree. This results indicate that the IMF B_y penetrates plasmoids and the magnetic structures must therefore be three-dimensional. In this note, the dynamical processes of magnetotail in the course of a substorm are studied using a MHD code with two-dimensions and three components on the basis of two types of initial equilibrium solutions of the quiet magnetotail. The numerical results of two cases illustrate various features of time evolution of B_y component that correspond to two kinds of plasmoid-like structures: one is associated with a flux rope core and the other resembles a “closed loop” plamoid. Therefore, the occurrence of various magnetic structures in the magnetotail might be related to nonsteady driven reconnection with different distributions of the B_y component.     

单晶炉勾形磁场设计参数实验验证

通过模拟方法得到8英寸单晶炉（16英寸坩埚）勾形磁场的设计参数,并对磁场参数的模拟结果进行了实验验证.结果表明：磁场参数及其分布均满足晶体生长要求,磁场参数的模拟结果与实验结果吻合较好.该模拟方法可用于勾形磁场的实际设计.     

Continuous lobe reconnection in the mid-tail and its relationship to substorms： Cluster observations of continuous lobe reconnection in the mid-magneto tail

When the IMF turns southward, a great amount of magnetic energy is stored in the magnetotail, and the electric field across the magnetotail substantially enhances. As long as magnetic reconnection （MR） in the magnetotail initiates and continues, the magnetic field and plasma in the central plasma sheet are carried away to the near-Earth and down to the tail, the magnetic field and plasma in the lobe region enter the CPS and are involved in MR. We call this process “Continuous Lobe Reconnection （CLR）”. In this paper a detailed analysis of Cluster observation of MR through 2001--2003 is made. Plenty of CLR events are found that led to considerable changes of tail configuration, appearance of BBF, as well as large-scale bubbles in which both plasma temperature and number density substantially decrease. It is shown that in general CLR events last for dozens of minutes and have good correspondence to substorm initiation under the condition of continuous southward IMF.     

亚暴期间场向电流的特征

分析了由ISEE-1和ISEE-2飞船在亚暴期间观测到的场向电流的特性,包括场向电流所伴随的行星际磁场、地方时与L值分布以及场向电流强度和密度随亚暴位相的变化,并着重分析了亚暴电流楔的特征。结果表明,亚暴膨胀相的场向电流强度和密度都达到极大值;亚暴的膨胀相是由行星际磁场转向或南向分量变小触发的,其起始位置很可能位于近地等离子体片内边缘。     

Correlation between continuous lobe reconnection in the mid magnetotail and substorm expansion onset

Data on plasma sheet crossing measured by Cluster/HIA and Cluster/FGM during the period from July to October in 2001 -2003 are analyzed. Based on previous work on the characteristic features of continuous lobe reconnection (CLR) described in reference, two case studies and a statistical analysis were carried out on correlation between CLR in the mid magnetotail and substorm expansion onset for the events occurring during this period. It is found that almost all CLR events are in close connection with substorms. The beginning of CLR is almost always a few minutes ahead of substorm activities seen in the near Earth magnetotail and on the ground-based stations. This provides a clear indication that CLR is the virtual cause of substorm expansion onset during the period of continuous southward interplanetary magnetic field.     

一种基于优化阈值函数的EEMD改进降噪方法

以提高降噪效果为目的,提出了一种基于白噪声分解特性的EEMD优化阈值降噪方法。避免了小波分解时选择合适小波基函数的困难,具有自适应性,同时,也可以有效地避免频率混叠问题。方法从能量密度和对应平均周期乘积的变化率出发,提出了“跳变点”和“奇异点”的选择原则,并利用优化阈值函数对“跳变点”和“奇异点”对应的IMF分量进行量化处理,然后通过对处理后的IMF分量重构得到降噪信号。最后用仿真信号进行试验,证明本方法的有效性和优越性。     

A UNIFIED MODEL FOR SOLAR FLARES

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非对称勾形磁场的三维优化设计与实现

根据坩埚内熔体对流的类型和分布区域,分析控制对流对勾形(cusp)磁场磁感应强度和磁场位形分布的要求,提出了磁场优化设计目标。采用有限元三维(3D)建模法对cusp磁场进行了建模,利用所建立的模型对比了对称结构和非对称结构对磁场位形分布的影响,分析了在非对称cusp磁场线圈横向层数一定的情况下磁场纵向层数、屏蔽体厚度、上下线圈间距对磁感应强度、磁场位形、磁场功率的影响,优化了磁场结构;根据优化的结构参数制造了磁场并进行了实验测试,结果表明非对称cusp磁场的位形分布与设计结果一致,从而验证了3D优化建模方法的有效性。     

Comparison of a new model with previous models for the low-latitude magnetopause size and shape

In this study, the advantages and the limitations of previous low-latitude magnetopause empirical models are discussed. In order to overcome their limitations and inherit their advantages, a new continuous function for the influence of the interplanetary magnetic field (IMF) Bz on the magnetopause, the Shue model function and the 613 low-latitude magnetopause crossings are used to construct a new low-latitude magnetopause model parameterized by the solar wind dynamic pressure (Dp) and IMF Bz. In comparison ...     

高海拔对火灾燃烧特性影响的试验研究

为研究高海拔对于火灾燃烧特性的影响,采用火灾试验研究的方式分别在高海拔地区和内地进行了火灾的燃烧试验,测得了不同尺寸油盘火源试样的燃烧时间和热释放速率,通过对比试验结果分析得到:高海拔地区火灾燃烧热释放速率相比内地较小,但是燃烧时间远比内地长,燃烧的火焰高度更高。     

基于脉间中断调频连续波的高空慢速单基机载SAR成像

调频连续波用于高空慢速单基机载SAR成像时,收发隔离和远距离探测都是亟待解决的问题。结合高空慢速运动平台的特点,提出了一种脉间中断调频连续波(Inter-Pulses Interrupted Frequency-Modulated Continuous Wave, IPIFMCW)的信号模型,通过载频不同的门控信号调制多个发射信号,设置较大的脉间中断时间,将子脉冲回波差频信号在快时间域时移合成大带宽信号,实现高空慢速机载SAR成像。通过与脉间中断调频连续波(FMICW)的理论分析比较,说明该方法不仅解决了收发隔离难题,同时满足高空机载SAR远目标成像需求,避免出现距离模糊。最后结合频率变标算法(FSA)实现了基于IPIFMCW信号的高空慢速单基机载SAR成像。     

Statistical survey on the magnetic field in magnetotail current sheets: Cluster observations

The distribution properties of the magnetic field in magnetotail current sheets have been explored statistically with the magnetic measurement data of the Cluster mission from June to November of the years 2001–2005. It is found that, on average, the strength of the magnetic field and its B_z component in the current sheet are weaker in the region close to midnight but stronger near the dawnside and duskside flanks, which implies that, in general, a thinner current sheet occurs near midnight and thicker ones near both flanks. The occurrence of tail current sheet flapping is higher on both flanks than in the midnight region, although it is most frequent in the dawn flank. Current sheets with a negative B_z component or a strong B_y component have a higher probability of occurring at magnetic local times of 21:00–01:00, indicating that magnetic activity, e.g. magnetic reconnection and current disruption occur more frequently there. Statistically, the probability distributions of the B_y component and the tilt angle of magnetic field lines in the current sheet are approximately normal distributions, and the occurrence probability of the flattened current sheet is about one third that of the normal current sheet. The magnetic field and B_z component in the current sheet mainly vary from 1 nT to 10 nT. The B_y component in the tail central current sheet is on average twice the IMF B_y at 1 AU.