大功率长偶极与环状电流源电磁波响应特征对比

为了在深部第二成矿带找矿,需要进一步提高电磁法可控源的强度,因此,一种新的大功率固定发射源的电磁法正在孕育之中.该方法采用长偶极源或者环状电流源,为了提高发射源的强度,偶极长度L或者环状源半径R需要非常大.然而,电磁场信号的强度不仅仅依赖于发射源,当L或者R为数十公里时,接收点的位置远离发射源,电离层对电磁场的影响不可以忽略.电离层的影响既可能是增强信号,也可能是削弱信号,这依赖于不同类型源产生的电磁波.本文利用三维积分方程法对包含电离层、空气层、固体地球层(简称地-电离层模型)的线状和环状大功率电流源电磁波响应进行了三维数值模拟,对两种源的电磁波的响应特征进行了对比研究.研究表明虽然磁性源的发射效率高于电性源,但是由于发射源在波导区产生的直达波经电离层的反射波要产生相长相消干涉,波导区的场特征既和发射源的特征有关,也和电离层有关.对比研究发现对于x方向的水平长偶极源电离层对电磁场 E_x 和 H_y 的影响是使场的幅值增强,即波导场的 E_x 和 H_y 的衰减是减缓的.而对于水平环状电流源,电离层对水平方向的电磁场的影响是使场的幅值减弱,即波导场的 E_x 和 H_y 的衰减是增大的.为此,认为采用大功率固定源在波导场工作时应该采用线状电流源.     

地磁脉动Pc5在2000年7月15～16日磁暴期间的特征

采用IMAGE链22个台站的地磁脉动10 s数据，分析了2000年6月15～16日磁暴期间Pc5地磁脉动的频率、振幅、位相和极化特征：（1）磁暴初相和主相期间Pc5脉动的主频率随纬度的升高而降低，但是恢复相期间主频率随纬度的升高而升高，主相期间Pc5的主频率比初相和恢复相期间的低；（2）Pc5脉动初相期间的振幅有一个主峰在64°N附近，主相期间在66°N附近，恢复相期间在71°N附近；位相在主峰两侧随着纬度变化了大约180°， 从初相到恢复相主峰位置向高纬地区大约移动了7°；（3）Pc5地磁脉动的偏振极化椭圆初相期间在PEL站（6346°N）接近线偏振，主相期间在MAS站（6607°N）接近线偏振，恢复相期间在BJN站（7133°N）接近线偏振，并分别在这几个台站两侧的偏振椭圆的旋转方向反向.     

海浪引起的地磁场波动的观测与初步分析

近岸海浪是影响近岸水域环境状态的重要环节.海洋近岸波的波动性质和变化规律的研究对于海岸防护、近岸航运、军事活动等具有重要意义.感应磁场波动可为探测海洋近岸波的非线性过程提供一种有效手段.本文首次对海洋近岸波引起的感应磁场进行了频谱指数分析,获得了能量注入和耗散过程对应的谱段.2016年5月15日—6月30日在昌黎海岸(东经119.3,北纬39.7°)利用KDM-2型磁通门磁力仪对海洋近岸波引起的磁场变化进行了测量,数据分辨率为0.01 nT/(HZ)~(1/2),时间采样率为1 Hz和128 Hz.观测数据显示,在距海岸线2 m远处,清晰地观测到了海洋近岸波引起的磁场波动,在0.001~10.0 Hz频段的波动最大振幅约为1 nT.波动的小波频谱呈现出多次谐波结构,符合海洋近岸波的谐波特征.傅里叶频谱显示不同频段谱的斜率不同,反映了海洋近岸波发展与耗散的非线性物理过程,进一步开展长期观测和统计分析有助于深入了解海洋中的电动力学过程.     

Long duration Pc 5 compressional pulsations inside the Earth’s magnetotail lobes

Pc 5-type magnetic field pulsations are detected by the IMP-8 spacecraft well inside the Earth’s magnetotail lobes. The three studied events with an average duration of 3 h and mean amplitude of B/B=6.6% show a strong longitudinal oscillation. The clockwise polarization sense of the magnetic field arrowheads in the north lobe (as well as the counterclockwise in the south lobe) on the XZ plane is consistent with that expected when periodic solar wind lateral pressures squeeze the magnetotail axisymmetrically while moving tailward. In the two case studies, the latter property has been found to concur with quasi-periodic upstream density fluctuations detected by ISEE-3 and/or ISSE-1. The lobe magnetic field oscillations are classified in two distinct modes. The manifestations of the first mode are tailward-travelling waves detectable along the B_y and B_z magnetic field traces (i.e., with regard to the B_z the spacecraft encounters constantly the same conspicuous signature of south-then-north tilting of field lines around each local compression region). The second mode is associated with prolonged periods of extremely low geomagnetic activity and exhibits a signature along the B_y component inconsistent with travelling waves. Thus, the maxima of compressions occur simultaneously with the maxima of B_y excursions: a feature that is explained in terms of tail-aligned current density flowing at the boundary which separates the stable magnetic field in the tail lobe from the very irregular in the magnetosheath. In this case, the spacecraft was located in the vicinity of the high-latitude tail boundary and the observed B_y excursions are consistent with those anticipated by the tail-aligned current polarity, which is determined by the dominant B_y-component of the interplanetary magnetic field (IMF). On the plane YZ we observe an almost linear and circular polarization sense of the vector magnetic field for the first and second mode, respectively.     

水平分层孔隙介质中点源激发的震电波场数值模拟及分析

为认识地震波诱导的电磁场的特性,本文研究地震波在孔隙介质中由于动电效应引起的电磁场.基于Pride弹性-电磁耦合方程组推导了双力偶震源对应的位移-应力-电磁场间断向量的表达式,模拟了双力偶源激发的震电波场.作为比较,还模拟了爆炸点源激发的震电波场.结果表明：存在伴随纵波的电场,其各分量的波形与固相位移对应分量的波形相似,但相位相反;存在伴随横波的磁场,其波形与固相位移波形相似;双力偶震源还激发出了独立传播的辐射电磁场,其速度比纵波至少高一个数量级,几乎是“瞬间同时”到达了每个接收器,但是其强度比伴随电磁场小得多,且随着源距增大而迅速减小.本文研究还表明：伴随纵波的电场强度不仅与地震纵波幅度和动电耦合系数有关,还与由介质孔隙结构决定的流-固两相动力协调性有关,存在一种动力协调介质,纵波在这种介质中不引起电场.     

反向消磁条件下磁流变脂隔震模拟试验研究

采用电磁线圈及永磁体共同控制磁场,自主设计一种可反向消磁的磁流变脂(MRG)剪切试验装置。利用ANSYS Electronics软件对该试验装置磁场分布进行仿真分析,并制备不同羰基铁粉质量分数的MRG,采用振动台对反向消磁条件下MRG的动态剪切性能开展试验测试,分别研究励磁电流、激振幅值和激励频率对MRG动态性能的影响。结果表明:羰基铁粉质量分数对MRG的动态性能影响显著;MRG的剪切应力随励磁电流的增大先快速增大后趋于平缓,阻尼力则逐渐减小;MRG的耗能能力随位移幅值的增加而增强;随着加载频率的增大,其阻尼力略有增加。     

迭部5.9级地震爆破地震波动力学特性的变化

本文利用遥测传输台网可见记录和磁带记录对厂坝炮爆破进行地震波动力学特性分析,发现各次爆破记录有一致性。对失真信号进行滤波处理,经凝聚函数分析证明了爆源的一致性。对1987年1月8日迭部Ms=5.9地震的分析,表明由于介质状态的改变,记录到的地震波优势频率向高频方向移动。在近震中有关台站上,地震波位移谱出现多峰与能量分散现象,拐角频率也向高频方向移动,振幅比呈现低—高—发震的形态。在地震前二十几天,主频处地震波衰减小,而震后明显变大。上述特征可能与该地震孕育过程中应力水平和介质状态变化有关。     

2007年3月3日长时间持续Pc5 ULF波的多点联合观测分析

2007年3月3日位于磁层昏侧THEMIS的5颗卫星、同步轨道晨侧和午前的GOES 3颗卫星和地面地磁台站同时观测到了持续近4 h的Pc5 ULF波.我们用交叉小波相关分析计算脉动的传播速度,用MVA分析求解脉动的传播方向,然后结合两者的计算结果获得了Pc5相速度矢量信息.THEMIS卫星观测到Pc5具有压缩特性,且向阳传播,速度约在6~20 km/s左右,相比于磁层中阿尔芬速度(1000 km/s)较低.这些Pc5 ULF波动可能产生于磁尾或磁层内部不稳定性.GOES 3颗卫星观测到不同情况的Pc5 ULF波,极向模占主要成分,且具有波包结构,具有阿尔芬驻波特性,可能产生于K-H(Kelvin-Helmholtz)不稳定性.地面台站观测到ULF波扰动幅度随纬度升高而增强,Pc5脉动在地理纬度60°附近达到最大值, Dumont durville台站观测到的脉动与THEMIS观测到波形有很好的相似性.     

Non-linear dynamo waves in an incompressible medium when the turbulence dissipative coefficients depend on temperature

Non-linear - dynamo waves existing in an incompressible medium with the turbulence dissipative coefficients depending on temperature are studied in this paper. We investigate of - solar non-linear dynamo waves when only the first harmonics of magnetic induction components are included. If we ignore the second harmonics in the non-linear equation, the turbulent magnetic diffusion coefficient increases together with the temperature, the coefficient of turbulent viscosity decreases, and for an interval of time the value of dynamo number is greater than 1. In these conditions a stationary solution of the non-linear equation for the dynamo waves amplitude exists; meaning that the magnetic field is sufficiently excited. The amplitude of the dynamo waves oscillates and becomes stationary. Using these results we can explain the existence of Maunders minimum.     

Observations of Pc5 micropulsation-related electric field oscillations in the equatorial ionosphere

A 54.95-MHz coherent backscatter radar, an ionosonde and the magnetometer located at Trivandrum in India (8.5○N, 77○E, 0.5○N dip angle) recorded large-amplitude ionospheric fluctuations and magnetic field fluctuations associated with a Pc5 micropulsation event, which occurred during an intense magnetic storm on 24 March 1991 (A_p=161). Simultaneous 100-nT-level fluctuations are also observed in the H-component at Brorfelde, Denmark (55.6○N gm) and at Narsarsuaq, Greenland (70.6○N gm). Our study of the above observations shows that the E-W electric field fluctuations in the E- and F-regions and the magnetic field fluctuations at Thumba are dominated by a near-sinusoidal oscillation of 10 min during 1730–1900 IST (1200-1330 UT), the amplitude of the electric field oscillation in the equatorial electrojet (EEJ) is 0.1-0.25 mV m⁻¹ and it increases with height, while it is about 1.0 mV m⁻¹ in the F-region, the ground-level H-component oscillation can be accounted for by the ionospheric current oscillation generated by the observed electric field oscillation in the EEJ and the H-component oscillations at Trivandrum and Brorfelde are in phase with each other. The observations are interpreted in terms of a compressional cavity mode resonance in the inner magnetosphere and the associated ionospheric electric field penetrating from high latitudes to the magnetic equator.     

Sensitivity of tidal sand wavelength to environmental parameters: A combined data analysis and modelling approach

An integrated field data-modelling approach is employed to investigate relationships between the wavelength of tidal sand waves and four environmental parameters: tidal current amplitude, water depth, tidal ellipticity and median grain size. From echo sounder data at 23 locations on the Dutch continental shelf, the average wavelengths of observed sand waves are determined and compared with the wavelengths obtained with a process-based model. The latter describes the initial formation of these bedforms due to feedbacks between the tidal current and the erodible bed and uses environmental parameters for the 23 locations as input. Good agreement between observed and modelled wavelengths is found if the bottom stress experienced by tidal currents is adequately quantified. Model results show that the wavelength of sand waves increases with increasing water depth, tidal ellipticity and grain size (coarse sand), whilst it decreases with increasing tidal current amplitude and grain size (fine sand). Due to the limited number of stations and the fact that all four parameters change from location to location, the modelled relationships are only partly supported by the field observations.     

中纬电离层大尺度扰动的数值模拟

利用计算机模拟研究了不同条件下中纬电离层F区大尺度扰动的时空演变.当存在幅度约为5％的初始扰动时,Perkins不稳定性能发展成为大尺度电离层不均匀体.大气重力波能触发Perkins不稳定性,在更短时间内增长成为大幅度电离层振荡.非均匀局部电场结构也能产生局部电离层的大幅度扰动.本义的模拟表明,中纬电离层大尺度扰动主要表现为磁通管内等离子体沿磁力线的振荡.模拟结果与观测现象符合得很好.     

Modification of electron concentration in the ionosphere in the pump-wave plasma resonance region

We discuss the propagation of sounding radio waves in the inhomogeneous ionosphere, in the reflection area of which there are small-scale artificial magnetically-positioned irregularities. The propagation of radio waves in such an area, where the lateral dimensions of strongly elongated artificial irregularities are smaller than the wavelength, has a diffraction nature. It is shown that the calculation of diffraction parameters makes it possible to derive the amplitude of density irregularities and their relative area perpendicular to the magnetic field direction. Comparison of theoretical calculations with experimental studies on modification of the electron density altitude profile by heating of the ionosphere with midlatitude stand Sura showed that the relative area of the negative density perturbations can reach several percent.     

基于JUNO卫星WAVES仪器波动数据的木星磁层哨声波分析研究

等离子体波的空间分布在木星磁层高能电子动力学过程中起着重要的作用.现有大多数对木星磁层哨声波的观测仅限于|λ|≤15°的磁纬范围内,但是最新的JUNO卫星WAVES仪器提供的波动数据使得更高纬度、更广区域范围内的等离子体波动分布研究成为可能.本文通过对JUNO卫星WAVES仪器数据进行分析处理,详细研究了木星磁层哨声波的空间分布特性.观测表明,存在位于高LJ、高磁纬的木星磁层哨声波,它们广泛分布于距木星中心距离35～75个木星半径、磁纬为|λ|≤30°的空间区域.分析研究发现,WAVES仪器观测的木星磁层哨声波幅度一般为几个pT,远小于地球磁层哨声波的强度.木星磁层哨声波幅会随着LJ的增大缓慢增加,也会随着磁纬的减小趋向平缓变化.基于以上观测事实,本文利用指数幂函数分别拟合得到木星磁层哨声波幅随LJ和磁纬变化的经验模型.该模型将有助于精确理解哨声波对木星磁层高能电子动力学过程的重要影响.     

Proton interaction with quasi-electrostatic whistler mode waves in an inhomogeneous plasma (magnetosphere)

We study the interaction between energetic protons of the Earth’s radiation belts and quasi-electrostatic whistler mode waves. The nature of these waves is well known: whistler waves, which are excited in the magnetosphere due to cyclotron instability, enter the resonant regime of propagation and become quasielectrostatic, while their amplitude significantly increases. Far enough from the equator where proton gyrofrequency and transversal velocity increase the nonlinear interaction between these waves and energetic protons becomes possible. We show that plasma inhomogeneity may destroy cyclotron resonance between wave and proton on the time scale of the order of particle gyroperiod which in fact means the absence of cyclotron resonance; nevertheless, the interaction between waves and energetic particles remains nonlinear. In this case, particle dynamics in the phase space has the character of diffusion; however, the diffusion coefficients are determined by the averaged amplitude of the wave field, but not by its resonant harmonics. For real parameters of the waves and magnetospheric plasma, proton pitch-angle diffusion leading to their precipitation from the magnetosphere becomes essential.     

Observations of Pc 3–4 and Pi 2 geomagnetic pulsations in the low-latitude ionosphere

Day-time Pc 3–4 (≃5–60 mHz) and night-time Pi 2 (≃5–20 mHz) ULF waves propagating down through the ionosphere can cause oscillations in the Doppler shift of HF radio transmissions that are correlated with the magnetic pulsations recorded on the ground. In order to examine properties of these correlated signals, we conducted a joint HF Doppler/magnetometer experiment for two six-month intervals at a location near L = 1.8. The magnetic pulsations were best correlated with ionospheric oscillations from near the F region peak. The Doppler oscillations were in phase at two different altitudes, and their amplitude increased in proportion to the radio sounding frequency. The same results were obtained for the O- and X-mode radio signals. A surprising finding was a constant phase difference between the pulsations in the ionosphere and on the ground for all frequencies below the local field line resonance frequency, independent of season or local time. These observations have been compared with theoretical predictions of the amplitude and phase of ionospheric Doppler oscillations driven by downgoing Alfvén mode waves. Our results agree with these predictions at or very near the field line resonance frequency but not at other frequencies. We conclude that the majority of the observations, which are for pulsations below the resonant frequency, are associated with downgoing fast mode waves, and models of the wave-ionosphere interaction need to be modified accordingly.     

阿尔芬波动特征对卫星磁力仪零位标定的影响

磁通门磁力仪的零位偏移量在卫星轨道上会因诸多因素而发生改变.为此,基于剪切阿尔芬波动不改变总磁场强度这一特征的Davis-Smith方法被提出用于计算磁力仪的零位补偿.实际上,行星际空间中没有纯粹的阿尔芬波动.本文采用数值模拟分析了存在小的压缩波动情况下,阿尔芬波动的幅度、周期和相位以及数据窗口时间长度等对Davis-Smith方法计算零位补偿的影响.我们发现,只有当阿尔芬波动的周期与压缩波动周期相同时,阿尔芬波动的性质会对零位补偿的计算产生不可忽视的误差.阿尔芬波动的幅度越大,零位补偿的误差越小.磁场各分量零位补偿的误差大小还会受到阿尔芬波动初始相位的影响.此外,数据窗口时间长度越长,则零位补偿误差趋于减小至真实值.     

Radio emission spectrum from an interplanetary shock front

The characteristics of low-damping high-frequency waves in hot magnetized solar and stellar coronal plasmas under the conditions when the electron gyrofrequency ω_He is equal to or higher than the electron plasma frequency ω_pe have been analyzed using the numerical solution of the dispersion equation. It is shown that the wave branches corresponding to the Z mode and ordinary waves approach each other when the magnetic field increases and become almost indistinguishable in a wide frequency range at all angles between the wave vector and magnetic field. A branch with anomalous dispersion appears at angles close to 90°. A new interpretation of broadband pulsations and spikes is suggested on the basis of the results.     

High-frequency waves in hot magnetized solar and stellar coronal plasmas

The characteristics of low-damping high-frequency waves in hot magnetized solar and stellar coronal plasmas under the conditions when the electron gyrofrequency ω_He is equal to or higher than the electron plasma frequency ω_pe have been analyzed using the numerical solution of the dispersion equation. It is shown that the wave branches corresponding to the Z mode and ordinary waves approach each other when the magnetic field increases and become almost indistinguishable in a wide frequency range at all angles between the wave vector and magnetic field. A branch with anomalous dispersion appears at angles close to 90°. A new interpretation of broadband pulsations and spikes is suggested on the basis of the results.     

磁通量浮现驱动磁场重联的数值研究

应用二维时变可压缩磁流体动力学数值模拟,研究了双极－单极磁场中由于磁通量浮现驱动的磁场重联过程．结果表明,双极场与单极场间磁力线的重联形成上升的冷而密的等离子体团,磁场演变成鞭状结构．向上运动的等离子体团到达其最大高度后将回落和弥散.等离子体团最大上升速度达０．１４ＶＡ,等离子体最大上升速度达０．２７ＶＡ,ＶＡ为下边界处的Ａｌｆｖｅｎ速度．随着磁通量浮现幅度的增大,等离子体上升速度增加,重联过程发展得较快．背景等离子体β１值（β１为等离子体压力与磁压之比）越小,等离子体团中密度增量越大．磁Ｌｕｎｄｑｕｉｓｔ数Ｓ在１０３－１０６之间的改变对等离子体的速度和密度增量影响并不明显．与电阻撕裂模不稳定性引起的自发重联相比,磁通量浮现会更有效地驱动双极－单极场中的磁场重联过程,寻致日冕Ｈα冲浪和Ｘ射线喷流的形成．