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基于磁异常进行场源边界识别(如断裂划分)是磁法勘探解释工作的重要内容.由于受到斜磁化、场源埋深、异常叠加以及噪声等多种因素的影响,基于磁异常直接进行场源的边界识别往往难以准确识别出场源体的边界,所以,人们研究了各种场源边界特征增强的方法技术,以便于进行场源边界的识别工作.近年来,国内外出现了很多新的边界特征增强方法,但有些方法的边界特征增强效果与已有方法相近,有的方法效果有待深化检验,存在验证方法的理论模型过于简单,未全面细致地分析出它们的优缺点等问题.针对上述情况,本文运用多种复杂、贴近实际的理论模型,深入对比分析了包括解析信号模法和倾斜角法等在内的15种具有代表性的边界增强方法,分析了它们在不同磁化方向、不同场源埋深、不同场源形态、异常叠加和噪声干扰等多种因素影响下的边界增强效果,重点归纳总结出它们的优缺点和适用条件,以为实际应用时的方法选择提供参考.通过模型实验,我们认为解析信号模垂向导数法、总水平导数法、解析信号模倾斜角法是在多种因素影响下,适用性较强、应用效果较好的三种方法. 相似文献
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在使用电偶极发射源的可控源电磁法(CSEM)勘探中,发射源的方位、长度、形状等对观测数据有重要的影响,然而现有的大部分三维数值模拟方法没有全面地将这些因素考虑进来,很多都只能应对非常简单的场源形态,例如单一方位的点电偶极子,这有可能显著降低模拟结果的准确性.本文实现了基于交错网格有限体积(FV)离散的海洋CSEM三维正演算法,能够模拟形态相对复杂的场源,包括任意方位的有限长直导线和弯曲导线发射源.该算法使用一次场/二次场方法,只需对二次场使用FV法求解,避免了场源的奇异性问题;一次场的计算为一维正演问题,使用准解析法求解,并且只要在计算一次场时考虑复杂的场源形态便可以实现同样场源的三维正演.通过与一维理论模型的解析解对比验证了三维程序的准确性,并针对三维理论模型进行了一系列正演测试,初步考察了场源形态对三维正演结果的影响. 相似文献
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《应用地球物理》2017,(1)
应用于煤矿巷道、工程隧道等地下有限空间以及城市和工程浅层探测的瞬变电磁法常采用多匝小线圈装置,但是多匝线圈装置的互感耦合大,关断时间长,使探测的浅部"盲区"增大。为此,提出了一种圆锥型场源装置,推导了该装置内各匝线圈半径的计算公式。采用理论解析式对均匀介质中圆锥型场源一次场、二次场特征进行了计算分析,对圆锥型场源与多匝线圈互感系数进行了比较;应用快速汉克尔变换和改进的余弦变换数值滤波法,基于叠加原理的思想讨论了圆锥型场源下瞬变电磁正演方法,并以H型和KH型地电模型为例对正演结果进行了"烟圈"反演分析。研究表明:对于等效磁矩为926.1A·m~2的多匝回线和圆锥型场源,前者的互感约为后者的9倍;增大圆锥型场源的高度可减小互感系数,但其底半径的进一步变化对互感影响有限。圆锥型场源一、二次场特征与多匝线圈相似,但其二次场和总场暂态响应强于多匝线圈。所提出的综合视电阻率方法适用于圆锥型场源计算,正演结果和"烟圈"反演结果与初始模型的吻合性良好。本文研究成果为减小瞬变电磁探测"盲区"提供一种选择,也为装置组合形式和非线性反演技术等后续研究提供理论参考。 相似文献
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大地电磁法一直以来基本都遵循场源为平面电磁波的假设,这种假设普遍适用于中高频的大地电磁研究,但在具有显著非平面波场特性的区域或开展长周期大地电磁研究时,则对场源平面波的理论基础带来了挑战,若不满足理论假设,将会导致深部探测的可靠性降低,勘探目标定位风险增高.本文通过选择线状、片状及非规则场源模型来模拟极光电集流、赤道环电流和横向波动的波数场源,开展了大地电磁场源效应的模拟研究,对比分析了非平面波模式和平面波模式的响应差别.模拟表明大地电磁场源效应强度与模型平均电阻率正相关,与频率和测点与源水平距离负相关,且与场源的高度、宽度和横向波长等参数均有关系,非平面波模式和平面波模式正演响应在一些情况下具有超过10％的差异.基于场源效应特征,归纳并提出了五种场源效应校正方法,一是计算极限模型来截断场源效应影响频段的频域截断法,二是对多个同步观测的邻近测点进行平均的测点平均法,三是延长测点观测时间的时间域延长法,四是剔除较强垂直磁场分量所对应场源效应较强段数据的时间域剔除法,五是直接考虑场源的反演,五种方法均能一定程度上降低大地电磁场源效应的影响.对于受场源效应影响的大地电磁数据,若直接采用平面波方式进行反演则可能在深部产生较大畸变,若在获知场源相关参数的基础上,可开展考虑场源的大地电磁反演来消除场源效应影响. 相似文献
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基于不同测量高度重力场及其梯度数据可同时对应同一场源并用于反演场源位置的分析原理,拓展不同高度场数据在欧拉反褶积法中的应用范围.首先,立足于对欧拉反褶积方法的理论研究基础,提出不同高度数据融合联合欧拉反演公式.其次,在理论模型上对多种高度数据联合反演做了测试分析计算,验证了不同高度场数据融合联合欧拉反褶积法能够改善位场解释中单一观测面数据计算带来的解的发散问题,收敛过程由此改善.最后,将本文方法应用于龙门山地区实际重力数据的解释,获得了研究区断裂分布特征. 相似文献
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在地震预报的实践过程中，我们深深的体会到地震前兆场源关系的深入了解是十分必要的。虽然地震预报是世界性的难题，但是，只要我们在实践的基础上，能从理论上对这一演化物理问题有逐渐深入的认识，在一定的条件下，对某些地震做出中期和短临预报是很有可能的。本文以共和地震为例，对地震前兆场源关系的复杂性进行了初步的分析研究。其结果认为，正确的认识场源关系，以场求源，以源推场，场源结合，跟踪短临异常是实现短临地震预报的前提和基础。 相似文献
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目前,对于可控源电磁法各向异性介质2.5维问题,主要采用一次场、二次场分离的方法消除场源奇异性并降低截断边界对计算区域的影响.该方法数值计算精度高,但是很难适用于复杂地形条件下的数值模拟.针对复杂地形问题,基于总场的有限元方法表现出一定的优越性,然而,这种方法存在场源奇异性问题和截断边界问题.本文采用基于总场计算的方法对带地形的可控源电磁法2.5维各向异性介质进行模拟研究,推导了考虑电导率和介电常数各向异性的2.5维控制方程;引入网格加密-收缩算法降低场源奇异性的影响范围,提升数值计算效率;引入行波分解边界条件降低截断边界的影响;提出任意采样反傅里叶变换方法,快速、高精度地计算出空间域电磁场分量.理论模型数值算例中:首先,验证了本文算法的有效性;其次,对任意各向异性倾角产生的可控源电磁响应规律进行研究;最后,采用山丘模型对各向异性介质电磁场的响应规律进行了模拟和分析. 相似文献
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The effects of the solar eclipse of March 29, 2006, in the signals of ULF radio stations, in the intensity of regular radio noise at frequencies of 0.3–10 kHz, and in the number of atmospherics received in Yakutsk mostly from the west have been considered. The observations were performed using a multichannel parallel analyzer-recorder (11 channels in the frequency band 0.47–8.7 kHz), one-point lightning direction and range finder (0.3–100 kHz), narrow-sector radio noise direction-finder (0.3–10 kHz), recorder of signals from VLF radio stations, and broadband radio noise recorder (0.3–100 kHz). A GPS clock was used to synchronize a recorder of signals from VLF radio stations. The effect was observed in radio signals, radio noise, and number of atmospherics from the direction 270° ± 20° counted off clockwise from the north during the last stage of the eclipse (～ 1100–1200 UT), when the lunar shadow approached the line of the nighttime terminator and obscured part of the signal propagation path. The effect was observed as an enhancement of the received signals by a factor of ～1.2, a factor of ～1.4 increase in the number of atmospherics, and a change in the radio station phase values. 相似文献
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O. V. Mingalev I. V. Mingalev V. S. Mingalev M. L. Khodachenko 《Geomagnetism and Aeronomy》2009,49(5):574-581
The problem of a smooth field configuration, which should be an initial configuration in modeling (using the method of coarse particles) the problem of a stationary solar wind flow around a magnetic cloud in the case of a spatially two-dimensional statement (when a magnetic cloud is considered as a force-free magnetic cylinder with a finite radius) is considered. It has been indicated that such a statement is possible only when the magnetic field in the solar wind is parallel to the cylinder axis. The method for finding the magnetic field of a force-free cylinder with a finite radius, when some field component is specified and another component is determined based on this one (which makes it possible to construct fields with preassigned properties), has been proposed. The variant for constructing the initial field configuration in the transition region around a cylinder has been proposed. This variant makes it possible to gradually pass from homogeneous crossed fields in the solar wind to a force-free magnetic and zero electric fields within a cylinder, an electric field being potential and orthogonal to a magnetic field (in the reference system related to a magnetic cloud). 相似文献
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《Journal of Atmospheric and Solar》2008,70(5):687-707
This paper reviews quantitative analysis results of the energy transfer and dissipation processes in the GUMICS-4 global MHD simulation. Reconnection power dissipating magnetic energy, dynamo power transferring energy from plasma to the field, and energy flux transport across the magnetopause surface are all examined separately and shown to yield consistent results. This is used to argue that magnetic reconnection is the process controlling the energy transfer, even though it is not localized near the reconnection line. The most important factors controlling the reconnection efficiency are the interplanetary magnetic field (IMF) orientation and the solar wind speed, while the IMF magnitude and solar wind density play a lesser role. During northward IMF, the reconnection efficiency is larger for high speed and low IMF than for low speed and high IMF magnitude, even though the solar wind electric field in both cases is the same. Moreover, increasing pressure by increasing density has a different effect from equal increase of pressure by increasing the solar wind speed. Comparison with statistical observational results shows that the simulation results are in qualitative agreement with the observations, which significantly increases our confidence in interpreting the simulation results. 相似文献
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Yu. M. Mikhailova G. I. Druzhin G. A. Mikhailova O. V. Kapustina 《Geomagnetism and Aeronomy》2006,46(6):783-795
Results of studying the thunderstorm activity dynamics during the Pacific hurricanes in August and October 2001, using broadband recording of the time forms of atmospherics on Kamchatka, have been presented. The number of atmospherics per minute at simultaneously determined azimuths of their sources has been used as an example of thunderstorm activity. An analysis of data processing results has indicated (a) in the absence of hurricanes, the maximal atmospheric flux level (10 ± 4 pulse/min) was observed at night, and the daylight level was 3 ± 1 pulse/min; (b) thunderstorm activity increases at the stage of tropical depression regardless of depression development into hurricane; in this case the flux of atmospherics can increase to 250 pulse/min at night and can be widely variable (5–100 pulse/min) in daytime; (c) in the sate of hurricane maturity, the thunderstorm activity level is not higher than the background level. It has been indicated that IGWs in the Earth’s atmosphere and the lower ionosphere are caused by lightning strokes accompanied by shock waves during expansion of the lighning channel. The results obtained are of interest in studying anomalous effects in the natural electromagnetic field in the VLF band during increased seismic activity on Kamchatka. 相似文献
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V. A. Mullayarov L. M. Abzaletdinova V. V. Argunov A. A. Korsakov 《Geomagnetism and Aeronomy》2011,51(6):825-834
The specific features of a method for radiosounding the lower ionosphere over earthquake epicenters using LF electromagnetic
signals of thunderstorm sources (atmospherics) have been considered. The effects of shallow-focus earthquakes with magnitudes
larger than 4.0 and their precursors manifest themselves in amplitude characteristics of atmospherics. It has been assumed
that variations in the signal characteristics are related to disturbances in the lower ionosphere. According to the results
of azimuthal scanning, cross-sectional dimensions of disturbed regions, as a rule, correspond to the dimensions of the first
two Fresnel zones for signals at a frequency of 10 kHz. Azimuthal scanning also indicated that the positions of disturbed
regions during and before earthquakes could have a certain dynamics and differ from the projection onto the earthquake epicenter.
The ratio of the amplitudes of electric and magnetic signal components, in the variations of which seismic effects before
earthquakes can also be observed, has been considered. An analysis of the ratio makes it possible to increase the probability
of predicting earthquakes when using the characteristics of the electromagnetic signals of lightning discharges as an additional
method of complex monitoring of disturbances in the lower ionosphere caused by seismic processes. 相似文献
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The solar wind velocity distribution in the heliosphere is best represented using a v-map, where velocity contours are plotted in heliographic latitude-longitude coordinates. It has already been established that low-speed regions of the solar wind on the source surface correspond to the maximum bright regions of the K-corona and the neutral line of the coronal magnetic field. In this analysis, v-maps on the source surface for Carrington rotations (CRs) 1787-1795, during 1987, have been prepared using the interplanetary scintillation measurements at Research Institute of Atmospherics (RIA), Nagoya Univ., Japan. These v-maps were then used to study the time evolution of the low-speed (\leq450 km s−1) belt of the solar wind and to deduce the distribution of solar wind velocity on the heliospheric current sheet. The low-speed belt of the solar wind on the source surface was found to change from one CR to the next, implying a time evolution. Instead of a slow and systematic evolution, the pattern of distribution of solar wind changed dramatically at one particular solar rotation (CR 1792) and the distributions for the succeeding rotations were similar to this pattern. The low-speed region, in most cases, was found to be close to the solar equator and almost parallel to it. However, during some solar rotations, they were found to be organised in certain longitudes, leaving regions with longitudinal width greater than 30○ free of low-speed solar wind, i.e. these regions were occupied by solar wind with velocities greater than 450 km s−1. It is also noted from this study that the low-speed belt, in general, followed the neutral line of the coronal magnetic field, except in certain cases. The solar wind velocity on the heliospheric current sheet (HCS) varied in the range 300–585 km s−1 during the period of study, and the pattern of velocity distribution varied from rotation to rotation. 相似文献
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High-performance computational models are required to make the real-time or faster than real-time numerical prediction of adverse space weather events and their influence on the geospace environment. The main objective in this article is to explore the application of programmable graphic processing units (GPUs) to the numerical space weather modeling for the study of solar wind background that is a crucial part in the numerical space weather modeling. GPU programming is realized for our Solar-Interplanetary-CESE MHD model (SIP-CESE MHD model) by numerically studying the solar corona/interplanetary solar wind. The global solar wind structures are obtained by the established GPU model with the magnetic field synoptic data as input. Meanwhile, the time-dependent solar surface boundary conditions derived from the method of characteristics and the mass flux limit are incorporated to couple the observation and the three-dimensional (3D) MHD model. The simulated evolution of the global structures for two Carrington rotations 2058 and 2062 is compared with solar observations and solar wind measurements from spacecraft near the Earth. The MHD model is also validated by comparison with the standard potential field source surface (PFSS) model. Comparisons show that the MHD results are in good overall agreement with coronal and interplanetary structures, including the size and distribution of coronal holes, the position and shape of the streamer belts, and the transition of the solar wind speeds and magnetic field polarities. 相似文献
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Lars O. Løseth 《Geophysical Prospecting》2011,59(1):145-160
In marine controlled‐source electromagnetic (CSEM) surveys the subsurface is explored by emitting low‐frequency signals from an electric dipole source close to the sea‐bed. The main goal is often to detect and describe possible thin resistive layers beneath the sea‐bed. To gain insight into how CSEM signals propagate, it is informative to study a stratified model. The electromagnetic field is then given in terms of integrals over TE‐ and TM‐polarized plane‐wave constituents. An asymptotic evaluation of the field integrals for large propagation distances results in explicit spatial expressions for the field components and the derived expressions can be used to analyse how the CSEM signals propagate. There are two major signal pathways in a standard CSEM model. One of these pathways is via the thin resistive layer and the resulting response is accounted for by a pole in the reflection response for the TM mode. The signal is propagating nearly vertically down to the resistor from the source, then guided while attenuated along the reservoir, before propagating nearly vertically up to the receiver. The response is slightly altered by the sea‐bed interface and further modified in shallow water due to multiple reflections between the sea‐surface and sea‐bed at both the source and receiver sides. The other major signal pathway is via the resistive air half‐space, the so‐called airwave. The airwave is generated by the TE mode and interacts with the subsurface via vertically propagating signals reflected between the sea‐surface and subsurface at both the source and receiver sides. 相似文献