磁暴期间几种主要磁扰成分的演化特征   总被引：6，自引：1，他引：5       下载免费PDF全文

吴迎燕  徐文耀  陈耿雄  陈博  刘晓灿 《地球物理学报》2007,50(1):1-9

本文利用中国地磁子午链台站的资料,对1997～1999年期间发生的25次磁暴,用自然正交分量法（NOC）、相关分析和傅里叶分析三种方法,分3个步骤依次分离出依赖于世界时（UT）的暴时变化（Dst）、依赖于地方时（LT）的太阳静日变化（Sq）和太阳扰日变化（SD）.对各种变化时空特征的分析表明：①Dst变化清楚地反映出赤道对称环电流磁扰的空间分布和时间演化特征;②满洲里、北京十三陵和琼中台Sq幅度在多数磁暴主相期间出现极大和极小值,反映了Sq焦点在纬度方向上的移动所产生的地磁效应;③SD变化在主相期间最强,在恢复相期间逐渐减弱;④相关分析和傅里叶分析提供了一种能有效提取Sq和SD变化的方法.  相似文献   

中国地磁台观测的2014年地磁急变          下载免费PDF全文

康国发  高国明  文丽敏  白春华 《地球物理学报》1954,63(11):4144-4153

地磁急变（jerk）是起源于地球外核并在导电地幔过滤效应后在地球表面观测到的一种地磁现象,其反映了地核内部某些动力学过程.Jerks在空间范围上既可以是区域性的,也可以是全球性的.中国地区地磁台能否检测到2014年jerk？针对这一问题,利用中国大陆10个地磁台的磁静日月均值和CHAOS-6全球磁场模型,分析了X、Y和Z分量2008—2018年期间的长期变化,估算了2014年前、后的长期加速度值,确定了2014年地磁jerk的时间和强度.研究表明中国地磁台Y分量的长期变化为"Λ"型,Z分量存在明显的"V"型,具有典型的jerk特点.Y分量jerk出现的时间大约在2014年6月,比非洲大陆的Algeria TAM台和南美洲French Guiana KOU台时间滞后大约4个月.这暗示着产生jerks的地核流体波动的时序特点.中国西部和东北部地磁台的长期变化形态有明显的差别,主要由非偶极磁场引起.CHAOS-6模型与地面台站的长期变化形态并非始终一致.本文结果有助于更好地理解和解释长期变化的时间演变和地理分布,并为深入探讨jerks的地核起源和驱动机制提供新的观测约束.  相似文献   

Forecasting geomagnetic activity     

R. P. Kane 《Pure and Applied Geophysics》1988,126(1):85-101

A study of the daily, monthly and annual values of the geomagnetic activity indexAp for 1932 onwards and of the annualaa indices for 1868 onwards indicated that their variations had large random components. Long-term predictions were not possible from time-series extrapolations.  相似文献   

Afternoon mid-latitude current system and low-latitude geomagnetic field asymmetry during geomagnetic storms     

A. Grafe  P. A. Bespalov  V. Y. Trakhtengerts  A. G. Demekhov 《Annales Geophysicae》1997,15(12):1537-1547

For four geomagnetic storms of middle intensity the relationship between the low-latitude magnetic field asymmetry using ASY indices and the intensity of the auroral eastward and westward electro-jet was considered. It was asked whether there exists a connection between ASY and the eastward electrojet. To answer this question equivalent current systems were estimated in mid-latitudes. It was found that the observations obviously show no correlative relationship between the low-latitude magnetic-field asymmetry and the eastward electrojet, whereas one exists between ASY and the westward electrojet. To explain the generally accepted common three-dimensional current system between the partial ring current and the eastward electrojet, a condensor model of the three-dimensional current system was developed. It could be shown that the short periodic variations of the partial ring current are shielded by the condensor and cannot influence the eastward-electrojet current.  相似文献   

地磁台站建设中磁测异常现象分析   总被引：1，自引：1，他引：0  

吴乔木 《地震地磁观测与研究》2006,27(4):63-66

地磁台建设磁性跟踪测试工作很重要,通过对跟踪磁测中发现的一个异常现象的分析,计算了不同重量、距离的铁磁性物质对磁房建筑场地磁场的影响,讨论了排除施工现场磁性干扰的一些办法,并得出各种重量铁磁性物质与磁房建筑物的安全距离,还讨论了地磁台部分建筑材料的选择问题。  相似文献   

Planetary distribution of geomagnetic pulsations during a geomagnetic storm at solar minimum     

N. G. Kleimenova  O. V. Kozyreva 《Izvestiya Physics of the Solid Earth》2014,50(1):102-111

We investigate the features of the planetary distribution of wave phenomena (geomagnetic pulsations) in the Earth’s magnetic shell (the magnetosphere) during a strong geomagnetic storm on December 14–15, 2006, which is untypical of the minimum phase of solar activity. The storm was caused by the approach of the interplanetary magnetic cloud towards the Earth’s magnetosphere. The study is based on the analysis of 1-min data of global digital geomagnetic observations at a few latitudinal profiles of the global network of ground-based magnetic stations. The analysis is focused on the Pc5 geomagnetic pulsations, whose frequencies fall in the band of 1.5–7 mHz (T ～ 2–10 min), on the fluctuations in the interplanetary magnetic field (IMF) and in the solar wind density in this frequency band. It is shown that during the initial phase of the storm with positive IMF Bz, most intense geomagnetic pulsations were recorded in the dayside polar regions. It was supposed that these pulsations could probably be caused by the injection of the fluctuating streams of solar wind into the Earth’s ionosphere in the dayside polar cusp region. The fluctuations arising in the ionospheric electric currents due to this process are recorded as the geomagnetic pulsations by the ground-based magnetometers. Under negative IMF Bz, substorms develop in the nightside magnetosphere, and the enhancement of geomagnetic pulsations was observed in this latitudinal region on the Earth’s surface. The generation of these pulsations is probably caused by the fluctuations in the field-aligned magnetospheric electric currents flowing along the geomagnetic field lines from the substorm source region. These geomagnetic pulsations are not related to the fluctuations in the interplanetary medium. During the main phase of the magnetic storm, when fluctuations in the interplanetary medium are almost absent, the most intense geomagnetic pulsations were observed in the dawn sector in the region corresponding to the closed magnetosphere. The generation of these pulsations is likely to be associated with the resonance of the geomagnetic field lines. Thus, it is shown that the Pc5 pulsations observed on the ground during the magnetic storm have a different origin and a different planetary distribution.  相似文献   

Variation of lunar and solar geomagnetic tides with sunspot and geomagnetic activity     

K. S. Raja Rao  S. Jeevananda Reddy 《Pure and Applied Geophysics》1973,111(1):2291-2299

Summary Solar and lunar geomagnetic tides inH at Alibag have been determined by spectral analysis of discrete Fourier transforms following the method of Black and the well-known Chapman-Miller method. The seasonal variation inL ₂(H) is opposite to that inL ₂(D) with maximum in thed season and minimum in thej season. In bothH andD the enhancement due to sunspot activity is larger in lunar tide than in solar tide. Surprisingly, the enhancement due to magnetic activity is greater inL ₂(H) than inS ₁(H), while the contrary is true for declination. It is inferred that there is a local time component of the storm time variation contrary to the view expressed by Green and Malin. The enhancements in amplitudesL ₂ andS ₁ inH andD, due to sunspot activity and due to magnetic activity, have been separated. The results show that the amplitude at zero sunspot number increases with magnetic activity in all the four parameters, while the enhancement due to sunspot activity at different levels of magnetic activity decreases with increase ofK _p. But if bothK _p andR are increasing, whenK _p increases enhancement due toR decreases and whenR increases enhancement due toK _p decreases.  相似文献   

Eccentric geomagnetic dipole drift     

Joseph C. Cain  Dave R. Schmitz  Christopher Kluth 《Physics of the Earth and Planetary Interiors》1985,39(4):237-242

A recalculation of the rate of westward drift of the eccentric geomagnetic dipole since 1900 has confirmed its correlation with irregularities in the excess length-of-day (LOD) as originally reported by Vestine. The major changes in the LOD curve since 1900 are shown to be well correlated with the westward drift rate from a number of magnetic models covering the interval. A new Magsat model of secular variation for 1980.0 shows no increase in the drift rate which dropped by a factor of three in the interval 1965–1970.  相似文献   

Spatial power spectra of the crustal geomagnetic field and core geomagnetic field     

Malcolm G. McLeod  Paul J. Coleman 《Physics of the Earth and Planetary Interiors》1980,23(2):P5-P19

Lowes (1966, 1974) has introduced the function R_n defined by $\text{R}{}^{\mathrm{n}}\text{=(n + 1)}\text{∑}\text{m=0}\text{∞}\text{[(g}{}^{\mathrm{m}}{}_{\mathrm{n}}\text{)}{}^2\text{+ (h}{}^{\mathrm{m}}{}_{\mathrm{n}}\text{)}{}^2\text{]}\text{where}\text{g}{}_{\mathrm{n}}{}^{\mathrm{m}}\text{and}\text{h}{}_{\mathrm{n}}{}^{\mathrm{m}}$ are the coefficients of a spherical harmonic expansion of the scalar potential of the geomagnetic field at the Earth's surface. The mean squared value of the magnetic field B = ??V on a sphere of radius r > α is given by $\text{〈}\text{B}\text{·〉 =}\text{∑}\text{n=1}\text{∞}\text{R}{}^{\mathrm{n}}\text{(}\text{a/}\text{r}\text{)}{}^{\mathrm{2n=4}}\text{where}\text{a}$ is the Earth's radius. We refer to R_n as the spherical harmonic spatial power spectrum of the geomagnetic field.In this paper it is shown that Rⁿ = R^M_n = R^C_n where the components R_n^M due to the main (or core) field and R_n^C due to the crustal field are given approximately by $\text{R}{}^{\mathrm{M}}{}_{\mathrm{n}}\text{= [}\text{(n =1)/}\text{(n + 2)}\text{](1.142 × 10}{}^9\text{)(0.288}{}^{\mathrm{n}}\text{Λ}{}^2\text{R}{}^{\mathrm{C}}{}_{\mathrm{n}}\text{= [}\text{(n =1){[1 — exp(-n/290)]/}\text{(n/290)} 0.52 Λ}{}^2\text{where}\text{Iγ = 1 nT}$. The two components are approximately equal for n = 15.Lowes has given equations for the core and crustal field spectra. His equation for the crustal field spectrum is significantly different from the one given here. The equation given in this paper is in better agreement with data obtained on the POGO spacecraft and with data for the crustal field given by Alldredge et al. (1963).The equations for the main and crustal geomagnetic field spectra are consistent with data for the core field given by Peddie and Fabiano (1976) and data for the crustal field given by Alldredge et al. The equations are based on a statistical model that makes use of the principle of equipartition of energy and predicts the shape of both the crustal and core spectra. The model also predicts the core radius accurately. The numerical values given by the equations are not strongly dependent on the model.Equations relating average great circle power spectra of the geomagnetic field components to R_n are derived. The three field components are in the radial direction, along the great circle track, and perpendicular to the first two. These equations can, in principle, be inverted to compute the R_n for celestial bodies from average great circle power spectra of the magnetic field components.  相似文献   

地球主磁场模型   总被引：13，自引：3，他引：10       下载免费PDF全文

白春华  徐文耀  康国发 《地球物理学进展》2008,23(4):1045-1057

主磁场建模是一项综合性的研究工作,它涉及主磁场理论、磁场测量、数据同化、模型表达、模型解释以及模型运用等多方面的研究.本文综述了近五十年来德国、丹麦和美英各国研究者提出的数十个地球主磁场模型,回顾了主磁场模型研究方面的进展,概述了模型的描述以及建模的理论基础和方法.  相似文献   

云南地磁台地震前地磁谐波振幅比分析   总被引：1，自引：1，他引：0  

郭明瑞  胡久常  王锡娇  郑在壮  马龙  吴佳林  王桂丹 《地震地磁观测与研究》2019,40(2):39-44

采用云南永胜和通海地磁台2010年1月至2018年12月记录的地磁分钟值数据,计算谐波振幅比随时间的变化,分析发现:2014年8月3日鲁甸6.5级地震、2018年9月8日墨江5.9级地震前,谐波振幅比曲线有2次明显下降—转折—恢复异常,分别于第1次异常恢复上升过程和第2次异常转折过程中发震,异常持续时间分别为3年和2年多,持续时间越长,震级越高;距震中较近的地磁台站谐波振幅比曲线出现不同步现象,即YZHx(NS)向与YZHy(EW)向的不同步及长短周期不同步。  相似文献   

Dynamic geomagnetic field models     

V. V. Kalegaev 《Geomagnetism and Aeronomy》2011,51(7):855-865

A review of modern dynamic models of the Earth’s magnetosphere (the A2000 paraboloid model and Tsyganenko’s T01 model) is presented. For the magnetic storm of January 9–11, 1997, the results of joint calculations of the magnetospheric magnetic field are presented and contributions of the large-scale magnetospheric currents to the D _st variations are analyzed. Both models were shown to be well consistent with measurement data; the contribution of the magnetotail current system to D _st is comparable to the contribution of the ring current. At the same time, the relative dynamics of magnetospheric current systems are different in different models. The differences in the magnetic field variation profiles for various current systems calculated by the A2000 and T01 models are explained by model parameterizations.  相似文献   

The geomagnetic field in 1996 according to measurements of the geomagnetic observatory wingst     

Günter Schulz 《Ocean Dynamics》1996,48(2):203-206

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拉萨地磁台地磁相对记录室磁场梯度对比分析     

旦增  次仁卓嘎  张治国  罗布占堆  小德吉 《地震地磁观测与研究》2011,32(3):67-71

测量拉萨地磁台观测区内自然地磁场梯度和建成地磁记录室后的地磁场梯度,并测量新建记录室内不同高度磁场梯度,对比分析新建地磁记录室内的磁场稳定性,进而找出潜在干扰源,并采取有效措施予以去除,为产出连续可靠的地磁相对记录数据提供环境条件.  相似文献   

地磁房湿度对地磁观测的影响及解决方案     

郅红魁  郭慧  耿淑芬  阴宏业  程楠  宋建锁 《中国地震》2015,31(2):409-414

地磁房湿度变化较快或过大都易引起地磁数据的异常变化,且室内湿度不易控制,地磁房、磁通门磁力仪探头湿度智能在线分析监控系统可以实时显示监控地磁房、磁通门磁力仪探头湿度的变化,超过湿度阈值则发出报警信号,进而可以采用科学的方法控制探头观测环境的湿度,提高观测数据的稳定性、可靠性。本文介绍了该系统的设计思路和主要功能。  相似文献   

地磁场水平梯度及高空地磁场的计算与分析   总被引：1，自引：0，他引：1  

冯彦  蒋勇  孙涵  安振昌  毛飞  柳士俊 《地球物理学进展》2013,28(2)

本文以2000.0年中国地区的实测数据为例,首先利用5阶Taylor多项式方法建立了各分量的地磁模型,接着对模型中各分量的纬度和经度进行微分,计算得到各分量的水平梯度值,并绘制了相应分量沿南北方向和东西方向的水平梯度分布图,最后通过Zmuda多项式方法,基于地面模型值以及水平梯度值计算了高空(100 km)的各分量磁场值,并分析了水平梯度分布规律以及各分量随垂直高度的变化.结果表明:地磁场北向分量X、垂直分量Z、总强度F和磁倾角Ⅰ分量的水平梯度主要随纬度变化,其中X、Z和F分量随纬度减少而梯度降低,东向分量y和磁偏角D分量的水平梯度不仅随纬度变化,而且随经度变化,F分量的南北向梯度值在我国中心地区最大.在垂直方向,X、Z和F分量的强度分别随高度的上升而近似线性减小,在100 km高度处,强度变化平均值分别为-4.629 nT/km、-15.368 nT/ km和-16.226 nT/km,y分量强度随高度上升而呈近似线性增加,其平均变化值为0.166 nT/km,而D和Ⅰ分量基本不发生变化.  相似文献   

The geomagnetic field in 1998 according to measurements of the wingst geomagnetic observatory     

Günter Schulz 《Ocean Dynamics》1999,51(1):105-108

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长春地磁台地磁场长期变化基本特征   总被引：7，自引：3，他引：4  

岳庆祥  于洪池  吴江星  孙旭丽  张晓强  杨海东  邹本良  张晓珠  刘灏 《地震地磁观测与研究》2004,25(2):75-78

长春地磁台从1957年开始进行正规地磁观测至今,地磁场的长期变化已完成了一个完整的下降、转折、上升的变化周期,这种长期变化是偶极场与非偶极场变化的叠加,以非偶极场变化为主体,并受东亚大陆磁异常场源强度及方向变化的控制和影响。  相似文献   

地磁正常场的选取与地磁异常场的计算   总被引：34，自引：8，他引：26       下载免费PDF全文

高金田  安振昌  顾左文  韩炜  詹志佳  姚同起 《地球物理学报》2005,48(1):56-62

根据2003年中国地磁观测数据（包括135年地磁测点和35个地磁台）以及我国邻近地区38个IGRF计算点的地磁数据,计算中国地磁异常场的分布。选取两种地磁场模型作为地磁正常场,一是国际参考地磁场的球谐模型,二是中国地磁场泰勒多项式模型。根据各个测点的地磁异常值（观测值减去模型计算值）,用球冠谐分析方法计算地磁异常场的球冠谐模型,并绘制2003年中国地磁异常（△D,△I,△F,△X,△Y,△Z）。分析和讨论了中国地磁异常场。  相似文献   

The solar causes of the occurrence of selected geomagnetic storms and geomagnetic quiet     

Bohumila Bednářová-Nováková 《Studia Geophysica et Geodaetica》1966,10(4):437-445

Резюме Приводится общее толкование возникновения геомагнитного покоя и геомагнитнЫх бурь на основании новЫх гипотез, разработаннЫх в Геофизическом институте ЧСАН. Приводятся некоторые случаи геомагнитного покоя. Что касается примеров геомагнитнЫх бурь, то здесь имеются в виду прежде всего такие бури, которЫе в литературе обозначаются как “проблема” бурь, далее бури для которЫх существует несколько иногда даже противоречивых толкований По рассматриваемому здесь способу можно бЫло бЫ истолковать любую геомагнитную бурю, равно как и небольшое возмущение. Для этого необходимоо располагать точным даннЫми относительно солнечной ситуации на ЦМ.

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Address: Boční II, Praha 4-Spořilov.  相似文献