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| 1 | 岩石破裂过程中的超低频电磁异常显示文摘震前电磁场和大地自电位的异常是重要的地震前兆现象.在零磁空间对超低频段的磁场和自电位的变化进行了岩石破裂的实验研究,细致地揭示出电场、磁场出现异常变化的全过程,对深入认识超低频电磁信号的微观机理具有重要的意义.实验发现,岩石受力后应变、电位和磁场的缓慢变化在空间分布上是首先在近破裂源处出现,继而随裂纹的发展而改变位置;在时间序列上先出现自电位异常,然后是超低频磁场的变化;在异常形态上,超低频电磁信号呈现出早期、中期、晚期3个阶段的明显差异.研究表明,岩石微破裂引起裂隙尖端处的电荷分离. 静电荷在局部区域的积累和运移,导致了自电位的脉冲状变化;而在主破裂阶段,积累电荷的急速运动形成瞬间电流,激发了脉冲式的磁场异常.本文详细介绍了这一综合实验的技术步骤和观测结果,并对地震电磁前兆的微观机理进行了探讨. | 郝锦绮 钱书清 高金田 周建国 朱涛 | 2003 | 地震学报2003，25，1： | 71 |
| 2 | Recent progress on ULF wave and its interactions with energetic particles in the inner magnetosphere显示文摘The global distribution properties of Ultra Low Frequency wave (ULF) in the inner magnetospgere and its interactions with energetic particles, such as the wave-particle resonance, modulation, and particle acceleration, are active topics in space physics research. These problems are fundamentally important issues to understand the energy transport from the solar wind into the magnetosphere. In this paper we briefly reviewed the recent research progress on ULF wave and its interactions with energetic particles in the inner magnetosphere; furthermore, we suggested some open questions for future study. | Theodore A. FRITZ | 2008 | Science China(Technological Sciences)2008，51，10： | 16 |
| 3 | Numerical study on ULF waves in a dipole field excited by sudden impulse显示文摘A three-dimensional numerical model is employed to investigate ULF waves ex-cited by the sudden impulse (SI) of the solar wind dynamic pressure interacting with a dipole magnetosphere. We focus on the solar wind-magnetosphere energy coupling through ULF waves, and the influences of the SI spectrum on the cavity mode structure and the energy deposition due to field line resonances (FLRs) in the magnetosphere. The numerical results show that for a given SI lasting for 1 min with amplitude of 50 mV/m impinging on the subsolar magnetopause, the total ULF energy transported from the solar wind to the magnetosphere is about the magni-tude of 1014 J. The efficiency of the solar wind energy input is around 1%, which depends little on the location of the magnetopause in the model. It is also found that the energy of the cavity mode is confined in the region near the magnetopause, whereas, the energy of the toroidal mode may be distributed among a few specific L-shells. With a given size of the model magnetosphere and plasma density distri-bution, it is shown that the fundamental eigenfrequency of the cavity mode and the central locations of the FLRs do not vary noticeably with the power spectrum of the SI. It is worth noting that the spectrum of the SI affects the excitation of higher harmonics of the global cavity mode. The broader the bandwidth of the SI is, the higher harmonics of cavity mode could be excited. Meanwhile, the corresponding FLRs regions are broadened at the same time, which implies that the global cavity modes and toroidal modes can resonate on more magnetic L-shells when more harmonics of the global cavity modes appear. | YANG Biao FU SuiYan ZONG QiuGang WANG YongFu ZHOU XuZhi PU ZuYin XIE Lun | 2008 | Science China(Technological Sciences)2008，51，10： | 12 |
| 4 | 电网静态等值方法的综合分析与评价显示文摘处理电力系统稳态问题的时候,网络静态等值常用来简化分析计算的复杂度,就其中的主要方法进行了较全面的阐述,系统地介绍了各种方法的分类、应用、基本原理以及演化过程,并着重对比论述了这些方法的优缺点。结论可以作为在实际应用中选择静态等值方法的依据。 | 李健 李栋 | 2006 | 电气应用2006，25，9： | 11 |
| 5 | Fast acceleration of “killer” electrons and energetic ions by interplanetary shock stimulated ULF waves in the inner magnetosphere显示文摘Energetic electrons and ions in the Van Allen radiation belt are the number one space weather threat. Understanding how these energetic particles are accelerated within the Van Allen radiation belt is one of the major challenges in space physics. This paper reviews the recent progress on the fast acceleration of 'killer' electrons and energetic ions by ultralow frequency (ULF) waves stimulated by the interplanetary shock in the inner magnetosphere. Very low frequency (VLF) wave-particle interaction is considered to be one of the primary electron acceleration mechanisms because electron cyclotron resonances can easily occur in the VLF frequency range. Recently, using four Cluster spacecraft observations, we have found that, after interplanetary shocks impact the Earth’s magnetosphere, energetic electrons in the radiation belt are accelerated almost immediately and continue to accelerate for a few hours. The time scale (a few days) for traditional acceleration mechanisms, based on VLF wave-particle interactions to accelerate electrons to relativistic energies, is too long to explain our observations. Furthermore, we have found that interplanetary shocks or solar wind pressure pulses, with even small dynamic pressure changes, can play a non-negligible role in radiation belt dynamics. Interplanetary shocks interaction with the Earth’s magnetosphere manifests many fundamental space physics phenomena including energetic particle acceleration. The mechanism of fast acceleration of energetic electrons in the radiation belt responding to interplanetary shock impacts consists of three contributing parts: (1) the initial adiabatic acceleration due to strong shock-related magnetic field compression; (2) followed by the drift-resonant acceleration with poloidal ULF waves excited at different L-shells; and (3) particle acceleration due to the quickly damping electric fields associated with ULF waves. Particles end up with a net acceleration because they gain more energy in the first half of this cycle than they lose in the second. The results reported in this paper cast a new light on understanding the acceleration of energetic particles in the Earth’s Van Allen radiation belt. The results of this study can likewise be applied to interplanetary shock interaction with other planets such as Mercury, Jupiter, Saturn, Uranus and Neptune, and other astrophysical objects with magnetic fields. | ZONG QiuGang WANG YongFu YUAN ChongJing YANG Biao WANG ChenRui ZHANG XiangYun | 2011 | Chinese Science Bulletin2011，56，12： | 11 |
| 6 | Multi-spacecraft observations of ULF waves during the recovery phase of magnetic storm on October 30, 2003显示文摘Based on observations obtained by Cluster C1, GOES 10, 12, and Polar, the global ULF wave properties are studied during the recovery phase of a very intense magnetic storm-Halloween storm (October 31, 2003, 21:00-23:00 UT). The results indicate that the ULF waves’ properties observed by different satellites, such as amplitude, period, etc. show large variations. This can be interpreted as that Field Line Resonance (FLR) might take place in the region where Cluster C1 passed. The compressional wave of the cavity mode coupled with FLR’s shear Alfven wave and fed energy to the latter, forming a large-amplitude toroidal mode. From the point of period, Cluster C1 observed the shortest period, GOES 10, 12 observed the middle, while Polar observed the longest. The wave period of toroidal mode observed by Cluster C1 kept almost unchanging when Cluster C1 passed L range from 11.7 to 5.3. Using the Squared Wavelet Coherence analysis method, we estimated that the FLR region in the dayside magnetosphere could expand to at least 4 local time widths. The toroidal mode observed by Polar was a standing wave, while the pol-oidal mode was a propagating wave, the observation results could be well ex-plained by the waveguide mode theory. Since the solarwind speed Vx was -800 km/s and the dynamic pressure varied little, we speculated that the source of the ULF wave was the Kelvin-Helmholtz instability at the magnetopause triggered by high speed solarwind. | YongFu Wang SuiYan Fu QiuGang Zong Biao Yang ZuYin Pu Lun Xie XuZhi Zhou | 2008 | Science China(Technological Sciences)2008，51，10： | 11 |
| 7 | 2010年元谋M_S 5.2地震前地磁极化异常研究显示文摘利用改进的地磁极化方法分析了2010年2月25日云南元谋M_S5.2地震前后楚雄、永胜、通海3个台站的地磁极化值变异系数CZH的变化特征。结果显示:震前3个月,楚雄台地磁极化值出现了显著的剧烈波动,变异系数CZH急剧增大,于震前两个月达到最大,约为正常变化值的2~3倍,震前一个月恢复正常,且该变化主要由垂直分量Z的剧烈波动引起。由于震级较小,在震中距较远的通海和永胜台不存在类似的变化。 | 姚休义 滕云田 | 2017 | 地震研究2017，40，3： | 8 |
| 8 | Ultra low frequency waves impact on radiation belt energetic particles显示文摘One of the most fundamental important issues in the space physics is to understand how solar wind energy transports into the inner magnetosphere.Ultra low frequency(ULF)wave in the magnetosphere and its impact on energetic particles,such as the wave-particle resonance,modulation,and particle acceleration,are extremely important topics in the Earth’s radiation belt dynamics and solar wind― magnetospheric coupling.In this review,we briefly introduce the recent advances on ULF waves study. Further,we will explore the density structures and ion compositions around the plasmaspheric boundary layer(PBL)and discuss its possible relation to the ULF waves. | ZONG QiuGang HAO YongQiang WANG YongFu | 2009 | Science China(Technological Sciences)2009，52，12： | 7 |
| 9 | Ultra low frequency waves observed by Double Star TC-1 in the plasmasphere boundary layer显示文摘The characteristic and properties of ULF waves in the plasmasphere boundary layer during two very quiet periods are present. The ULF waves were detected by Double Star TC-1 when the spacecraft passed through the plasmasphere in an outbound and inbound trajectories, respectively. A clear association between the ULF waves and periodic variations of energetic ions fluxes was observed. The ob-servations showed that the wave frequency was higher inside the plasmasphere than outside. The mechanism generating these ULF waves and possible diagnos-ing of the 'classical plasmapause' location with the ULF wave were discussed. | XIE Lun ZHANG XiaoJia PU ZuYin WANG YongFu FU SuiYan ZONG QiuGang | 2008 | Science China(Technological Sciences)2008，51，10： | 7 |
| 10 | Numerical simulation of magnetospheric ULF waves excited by positive and negative impulses of solar wind dynamic pressure显示文摘The sources of ultra low frequency (ULF) waves in the magnetosphere are generally believed to be either the external solar wind perturbations or the internal plasma instabilities. When a sudden impulse of the solar wind dynamic pressure impinges on the magnetopause, ULF waves might be excited and thus the solar wind energy is transported into the earth's magnetosphere. In this paper, we study the ULF waves excited by different kinds of sudden solar wind pressure impulses through an MHD simulation. We primarily focus on the responses of the earth's magnetosphere to positive/negative impulses of solar wind dynamic pressure, and positive-negative impulse pairs. The simulation results show that the ULF waves excited by positive and negative impulse have the same amplitude and frequency, with 180° difference in phase, if the amplitude and durations of the input impulses are the same. In addition, it is found that field line resonances (FLRs) occur at certain L-shell regions of the earth's magneto-sphere after the impact of different positive-negative impulse pairs, which appear to be related to the duration of the impulses and the time interval between the sequential impulses. Another result is that the energy from the solar wind could be transported deeper into the inner magnetosphere by an impulse pair than by a single pulse impact. The results presented in this paper could help us to better understand how energy is transported from solar wind to the earth's magnetosphere via ULF waves. Also, these results provide some new clues to understanding of how energetic particles in the inner magnetosphere response to different kinds of solar wind pressure impulse impacts including inter-planetary shocks. | ZHANG XiangYun ZONG QiuGang YANG Biao WANG YongFu | 2009 | Science China(Technological Sciences)2009，52，10： | 6 |
| 11 | 地震“ULF”电磁扰动接收原理及异常特征显示文摘经过多年辛勤的努力,地震预报取得了一定的进展,但具有实际意义的短临预报还有待解决。与地震相关的电磁异常现象近来被认为是一种有希望解决地震短临预报的有效方法。在宽频范围内已经积累了前兆信号事件,ULF现象是其中有效的方法之一,短期预报很有希望通过ULF方法来实现。本文主要介绍探测ULF电磁扰动方法的接收原理和异常特征。 | 肖武军 关华平 | 2006 | 地震地磁观测与研究2006，27，5： | 4 |
| 12 | Reconstruction of morningside plasma sheet compressional ULF Pc5 wave显示文摘We studied the compressional wave event in Pc5 frequency range observed in the dawn-side magnetic equator on 9 March 1998 by Grad-Shafranov(GS) reconstruction method for the first time. To test the effectiveness of application of GS method on Pc5 compressional wave, we benchmarked our procedure by applying it to a one-dimensional current sheet model first. Excluding the left-hand corners, the average error magnitude was less than 10%. The reconstruction of actual data showed that we obtained the 2-D map of compressional wave without suffering model constraints for the first time. The magnetic filed lines density cyclical changed, and the wavelength was about 2-4 times earth radius. The reconstructed magnetic topology had a shape very similar to the empirical 2-dimensional standing wave model proposed by the former workers. Besides, we also recovered the plasma thermal pressure and current density of the wave quantitatively. | TIAN AnMin ZONG QiuGang SHI QuanQi | 2012 | Science China(Technological Sciences)2012，55，4： | 4 |
| 13 | Multiple ground-based observations at Zhongshan Station during the April/May 1998 solar events显示文摘Simultaneous observations at Zhongshan Station, Antarctica, during May 1-7, 1998 are presented to show the responses of the polar ionosphere to the April/May 1998 solar events. One of the main geo-effects of the solar events resulted in the major magnetic storm on May 4. At the storm onset on May 2 the ionosphere F2 layer abruptly increased in altitude, the geomagnetic H-component started negative deviation and the spectral amplitude of the ULF wave intensified. Both large isolated riometer absorption and large negative deviation of the geomagnetic H-component occurred at about 0639UT. There was a time lag of about one hour and ten minutes between the storm onset and the IMF southward turning, as measured by the WIND satellite. The polar ionosphere was highly disturbed, as shown by frequent large deviations of the geomagnetic H-component, large riometer absorption events and strong ULF waves in all the courses of the storm. The absorption increased greatly causing the digisonde to be blackout most of the time. However, the data still showed a substantial decrease in the F2 electron density and oscillation of the F2 layer peak height with an amplitude exceeding 200 km. | 刘瑞源 胡红桥 贺龙松 刘勇华 刘顺林 李胜桂 N. Sato B. J. Fraser | 2002 | Science China Mathematics2002，45，z1： | 3 |
| 14 | 煤岩损伤破坏ULF电磁感应实验研究显示文摘利用建立的煤岩声-电信号测试系统,对强度较低的煤岩试样进行了单轴压缩、剪切加载破坏实验,测试研究了ULF(1 kHz)、VLF(5 kHz)、LF(300 kHz)等频段电磁辐射及42.3 kHz声发射(AE)信号规律,并初步探讨了煤岩变形破坏ULF电磁信号的产生机理。结果表明:煤岩材料在单轴压缩和剪切变形破裂过程中能够产生ULF频段的电磁信号;与LF及VLF电磁信号相比,ULF信号与应力的相关性更好;同时,ULF信号与应力及AE相比存在一定程度的超前性,一般超前应力及AE信号5~10 s。实验室测得的煤岩变形破裂产生的ULF电磁信号,主要是由电荷运动产生的感应场变化引起的,煤岩材料中含有的少量金属矿物成分导致的压磁效应也是其来源之一。煤岩ULF电磁信号的研究不仅扩展了煤岩电磁辐射技术的研究范围,而且由于其在传播距离和抗干扰能力方面的优势,有望对远距离和较大尺度范围的煤岩动力灾害监测技术实现突破。 | 王恩元 贾慧霖 李楠 宋大钊 | 2012 | 煤炭学报2012，37，10： | 2 |
| 15 | 与地壳活动有关的ULF地磁变化:RIKEN-NASDA项目概要和最新结果显示文摘尽管地震短临预报极其重要,并且经过了人们多年的努力,但它仍是目前未能解决的问题。近年来,与地震相关的电磁现象被认为是解决地震短临预报的有效途径之一。现在已经积累了大量的地震电磁前兆信号的震例,这些信号分布在很宽的频带范围(DC-VHF)内,其中ULF地磁变化是最有希望的地磁前兆之一。通过监测ULF地磁变化,有望实现地震短临预报。本文将阐述从ULF电磁信号中提取震磁异常变化的方法。 | K.Hattori I.Takahashi M.Hayakawa N.Isezaki K.Yumoto T.Nagao S.Uyeda 李琪 杨冬梅 | 2005 | 世界地震译丛2005，36，3： | 2 |
| 16 | 菲尔兹奖章获得者Cédric Villani访谈录显示文摘Ulf Persson(以下简写为“UP”):当你得知将成为菲尔兹奖获得者时,你的感觉如何?吃惊吗?Cédric Villani(以下简写为“CV”):确实有些吃惊,但这不是主要的情绪.是的,起初我怕这是一个玩笑,在真正感到喜悦之前我在等待证实.那确实是一个激动人心的时刻.一方面,我感到如释重负, | 赵振江(译) 陆柱家(校) | 2011 | 数学译林2011，30，2： | 1 |
| 17 | ULF electromagnetic precursors before the 1999 Jiji, Taiwan, earthquake and the comparison with results of simulating experiments显示文摘There are many reports about the abnormal electromagnetic signals observed before great earthquakes. In particular, the signals of electromagnetic anomalies before the Hyogo-Ken Nanbu, Japan, MS=7.2 earthquake on January 17, 1995 (Hayakawa, et al, 1996) and those before the Loma Prieta, USA, MS=7.1 earthquake on October 19, 1989 (Fraser-Smith, et al, 1990) are especially remarkable. However, what the above authors reported are only the phenomena of one or two observatories. In order to confirm this phenomenon, the authors studied the results obtained by nine observatories in the southeast coastal areas of Chinese mainland within a range of 256~858 km to the epicenter of the 1999 Jiji, Taiwan, earthquake using instruments of the same type (the ULF/VLF electromag-netic wave observation system). By summarizing the data for the three months up to the time of earthquake occur-rence, the authors obtained the regional distribution of the signals of electromagnetic anomalies before the earth-quake and their features in the time domain and frequency domain. | QIAN Shu-qing | 2001 | Acta Seismologica Sinica(English Edition)2001，14，3： | 1 |
| 18 | 晨侧等离子体片ULF Pc5压缩波的重构分析显示文摘本文首次使用Grad-Shafranov(GS)方法研究了1998年3月9日晨侧磁赤道附近ULFPc5压缩波事件.为了验证GS方法对ULF重构有效性,先用一维电流片模及其析检验了GS重构方法对开放磁力构重构效果,果表明除了边角磁势之外,整开放磁力构重构误差在10%以内.我们GS重构果首次给出了受任模约束压缩波二维图象,显示了磁力疏密交变化特征.进一定量出ULFPC5压缩波波长为2至4个地球半,磁场态与前人提出经验压缩波2维驻波模似.在本文重构中,仅重现了ULFPc5压缩波三个磁场分量分,还定量地重现了波场中热压强电流密度分. | 田安民 宗秋刚 史全歧 | 2012 | 中国科学:技术科学2012，42，6： | 1 |
| 19 | ULF electric and magnetic anomalies accompanying the cracking of rock sample显示文摘The anomalies of electric-magnetic field and self-potential before earthquakes are important precursory phenom-ena. A simulating experiment study on the variations in ultra-low frequency (ULF) magnetic field and self-poten-tial during rock cracking was carried out in a magnetic field-free space. The results revealing in detail the whole process of the occurrences of electric and magnetic anomalies are significant for understanding the microscopic mechanism of ULF electric and magnetic signals. The experiment indicated that at the initial stage the slow changes in strain, self-potential and magnetic field with small amounts appeared firstly near the source of initial cracking, and then extended as the crack developed on. In the time domain, the self-potential anomaly emerged first and ULF magnetic field changes arose then. The shape of the ULF electric and magnetic anomaly varied ob-viously in early-, mid- and late-term of the test. The authors attributed the pulse-like changes of self-potential to the generation and movement of the accumulated electric charges during the cracking caused by charge separation on the crack tips within the sample. While the magnetic pulses of shorter-period at the last stage of the test, may be induced by instantaneous electric current of the accumulated charge during the cracking acceleration. The technical method and the observational results of this experiment are given in detail and the microscopic mechanism of elec-tric and magnetic precursors before earthquake are discussed in the present paper as well. | 郝锦绮 钱书清 高金田 周建国 朱涛 | 2003 | Acta Seismologica Sinica(English Edition)2003，16，1： | 1 |
| 20 | Poleward-moving recurrent auroral arcs associated with impulse-excited standing hydromagnetic waves显示文摘In Earth's high-latitude ionosphere, the poleward motion of east–west elongated auroral arcs has been attributed to standing hydromagnetic waves, especially when the auroral arcs appear quasi-periodically with a recurrence time of a few minutes. The validation of this scenario requires spacecraft observations of ultra-low-frequency hydromagnetic waves in the magnetosphere and simultaneous observations of poleward-moving auroral arcs near the spacecraft footprints. Here we present the first observational evidence from the multi-spacecraft THEMIS (Time History of Events and Macroscale Interactions during Substorms) mission and the conjugated all-sky imager to support the scenario that standing hydromagnetic waves can generate the quasi-periodic appearance of poleward-moving auroral arcs. In this specific event, the observed waves were toroidal branches of the standing hydromagnetic waves, which were excited by a pulse in the solar wind dynamic pressure. Multi-spacecraft measurements from THEMIS also suggest higher wave frequencies at lower L shells (consistent with the distribution of magnetic field line eigenfrequencies), which indicates that the phase difference across latitudes would increase with time. As time proceeds, the enlarged phase difference corresponds to a lower propagation speed of the auroral arcs, which agrees very well with the ground-based optical data. | HuaYu Zhao Xu-Zhi Zhou Ying Liu Qiu-Gang Zong Robert Rankin YongFu Wang QuanQi Shi Xiao-Chen Shen Jie Ren Han Liu XingRan Chen | 2019 | Earth and Planetary Physics2019，3，4： | 1 |
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