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1.
使用华南地区5个国家基准地磁台2008—2018年地磁观测数据,通过对磁偏角D、磁倾角I、总强度F、北向分量X、东向分量Y、水平分量H、垂直分量Z月均值及年变率的分析,研究该区地磁场长期变化特征。结果表明,华南地区5个地磁台近10年来七要素月均值及年变率均呈缓慢变化趋势,且变化量相当,反映了该区域地磁场长期变化的特征。 相似文献
2.
本文使用2008-2010年三年内的国内41个地磁台站和国外4个地磁台站的地磁水平分量H和磁偏角D的分钟值数据,研究了H和D的Vr指数(以下简称VrH和VrD)与Kp指数的关系及其时空分布特征,发现在时间变化上,VrH和VrD均具有27天太阳自转周变化;VrD呈现出显著的季节变化,而VrH却无,但与太阳风速度(SWS, Solar Wind Speed)变化密切相关,其三年的相关系数分别是0.97、0.70、0.88;去除季节变化后的VrD也表现出与SWS的相关,相关系数分别是0.96、0.77、0.5(2010年相关系数低主要受3月份Vr指数不明原因异常变化影响).在空间变化上,在我国大陆范围内,VrH和VrD均随纬度的增高而增大,并且具有地方时效应和显著的晨-昏不对称性,这种地方时效应和晨昏不对称性可能与部分环电流和场向电流有关系.研究认为Vr指数可以反映地磁场的快速变化,并可以间接反映SWS、部分环电流和场向电流对地磁场变化的影响和控制作用. 相似文献
3.
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
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
4.
选用中国21个地磁基准台站2011年的绝对子夜均值数据,分析D、H、Z分量年变化量空间分布特征。结果显示,各分量年变化量等值线分布比较均匀,其中:D分量年变化量等值线大致沿南北向分布,零经线附近台站年变化量较小;H分量年变化量等值线大致呈U型分布,且中心点位于甘肃省;Z分量年变化量等值线沿纬线方向,随纬度减小而增大。 相似文献
5.
本文通过对中国地区地磁场的球冠谐和分析和曲面样条分析,建立了2010.0年代的"中国地磁参考场球冠谐和模型"和"中国地磁参考场曲面样条模型".得到如下结论:"2010.0年代中国地磁参考场球冠谐和模型"描述的各地磁要素空间分布与"2005.0年代中国地磁参考场球冠谐和模型"较相似,但局部略有变化.比如对于磁偏角D和东向分量Y大致可理解为负值区域增强;磁倾角I在我国华北、华南和东北大部大面积正异常区消失了,但在我国西北部大面积的负异常区仍然维持;总强度F和垂直分量Z整体的负异常分布仍然维持,新疆西部局部地区和东南沿海地区局部的正异常分布则略有变化;变化最大的是水平分量H和北向分量X的空间分布,在2010.0年代,东南地区出现了大范围的正异常区,而且在中国北部出现了一条东西条带状的正异常区,似乎可认为是2005.0年代存在于太平洋的正异常区向西移动扩大的结果."2010.0中国地磁参考场曲面样条模型"描述的磁偏角D和东向分量Y相对较为曲折,最显著的异常位于蒙古境内,其次为滇东北地区、东北及华北大部、新疆等地区;磁倾角I和垂直分量Z相对较为平缓,最显著的异常存在于蒙古境内,其次的异常在内蒙满洲里附近;总强度F、水平分量H和北向分量X最为显著的异常位于满洲里附近,其次的主要异常区位于新疆地区、京津附近、滇东北地区. 相似文献
6.
根据19360年426个地磁测点和28个IGRF计算的地磁数据,计算地磁场和地磁异常场各个分量的曲面Spline模型,并绘制相应的地磁图和地磁异常图.依据我国部分地区的1909～1915,1915～1920,1920～1930,1930～1936年间地磁偏角长期变化图,1908～1917,1917～1922,1922～1936年间水平强度长期变化图和1908～1922,1922～1936年间垂直强度长期变化图,使用曲面Spline方法,分别计算上述9个时间段的磁偏角（D）、水平强度（H）和垂直强度（Z）长期变化的曲面Spline模型,并绘制相应的长期变化图.根据这些长期变化模型,将19360年426个点的三分量绝对值数据归算至1940,1930,1920,1910年和1900年,从而为计算这5个年代的地磁场模型奠定了坚实的基础. 相似文献
7.
地磁场对1999年9月空间天气大事件的响应 总被引：1，自引：0，他引：1
王文 《地震地磁观测与研究》2001,22(6):13-17
1999年9月22－25日发生一个大磁暴（Dst=-164nT).磁暴主相开始的头1小时伴随有丰富的Pc型地磁脉动，包括Pc2,Pc3,Pc4等。在行星际磁场Bz由北向转向南向后，磁暴主相开始，南向分量达到最大值后大约2小时，地磁H分量达到最小值，恢复相开始，并且，这次磁暴与太阳风各参数以及星际电场也存在一定的对应关系。 相似文献
8.
本文采用小波变化分别对受磁扰时段的"天宫一号"大气质谱信号和乌鲁木齐台地磁FHDZ-M15秒数据进行频段分析.实验发现"天宫一号"大气质谱信号和地磁M15秒数据信号的频谱优势频段在0.005~0.025 Hz之内,其中主要受干扰的频段为0.01~0.02 Hz.在地磁M15秒数据的预处理数据中,将H分量和F分量的主要磁扰频段滤出,实验结果表明:含有主要磁扰频段的H分量和F分量SNR(信噪比)分别为37.17 d B和32.99 d B,滤出空间主要磁扰频段后的H分量和F分量SNR分别为215.71 d B和245.54 d B,SNR有了很大的提高.地磁M15秒数据信号有了较为明显的改善,提高地磁资料对于地震监控的应用效果. 相似文献
9.
10.
本文根据最新的国际地磁参考场模型(IGRF11),结合梯度法分析能够很好的表现细微变化部分特征的优点,计算和绘制了1900—2010年期间间隔5年的全球地磁场水平分量H的水平梯度和垂直梯度,分析其时空分布,各磁异常中心位置和强度的变化规律。结果表明,地磁场的各个异常中心位置在水平方向和垂直方向上都有变化,主要以西漂为主,南大西洋正磁异常区水平分量梯度异常中心点强度值变化最大。 相似文献
11.
《地震科学（英文版）》2010,(4)
By calculating the hourly standard deviation of the first-order differences of the horizontal geomagnetic component minute data,a new index Vr to represent the variation rate of the geomagnetic field was introduced.Vr-indices show similar trends in the temporal change at different observatories and have simultaneous peak values at the observatories covering a large span geographically,which reveals that the source of geomagnetic disturbances represented by Vr is in the magnetosphere.Based on the comparison among Vr,Kp and ap,it is found that generally Vr changes linearly with Kp and ap,which means that the rapid changes of magnetic field usually exist together with magnetic disturbances.But there are exceptions.As Vr can be easily produced by individual observatory in quasi real time and is more sensitive to the variation rate of geomagnetic field rather than the field itself,it can be expected to serve for monitoring or predicting the geomagnetic-induced event in a quick and intuitive way. 相似文献
12.
选取恩施台、涪陵江东台、石柱黄水台以及武隆仙女山台2012年1月至2017年11月地磁数据进行异常分析,得到各个台站的地磁谐波振幅比和加卸载响应比计算结果,并结合2017年11月23日重庆武隆M5.0地震震中附近地质构造背景分析地震前后地磁异常现象。分析结果认为大部分地磁谐波振幅比变化特征类似于地电阻率的变化特征,表现为"下降-转折-上升"过程。本次地震大致发生在转折上升的初期阶段,其中震中距较小的台站地磁谐波振幅比变化趋势不同步,但变化幅度大致相同,而震中距较大的台站地磁谐波振幅比变化趋势较为同步,变化幅度较大。此外,研究还表明震前地磁加卸载响应比异常高值在时空分布上与震中位置具有很好的对应关系。 相似文献
13.
《Journal of Atmospheric and Solar》2002,64(3):377-387
The occurrence of pearl-type (Pc 1) micropulsations recorded at the mid-latitude station Nagycenk (Hungary) during a half solar cycle showed a quite regular variation on this long time scale. Around solar activity maximum, the number of days with Pc 1 occurrence was rather low, while it began to increase during medium solar activity rising to a maximum around solar activity minimum. Pc 1 pulsations have been analyzed in relation to further parameters and on a shorter time scale, too. Based on data of 2 years with maximum Pc 1 occurrence (around solar activity minimum in 1985 and 1986), a seasonal variation was also found. Additionally, it was confirmed that pearl-type micropulsations might frequently occur, on and after days, with geomagnetic disturbances. At Nagycenk, the selected geomagnetic disturbances were generally associated with an increased ionospheric absorption of radio waves caused by enhanced ionization due to particle precipitation from the magnetosphere into the lower ionosphere. Whistler observations carried out at Panska Veš (a station in the Czech Republic) showed a significant whistler activity connected with these geomagnetic disturbances, however, no after-effect appeared in whistler activity. One of the main goals of the present study was to find a relationship between Pc 1 pulsations and whistlers. Results revealing an increased whistler activity associated with Pc 1 occurrences confirm our previous findings rather convincingly. The latter ones hinted at the probability that certain magnetospheric configurations, e.g. geomagnetic field line shells and whistler ducts are closely connected, as similar positions of the two structures were found within the magnetosphere when characteristics of Pc 3 pulsations and whistlers were analyzed. 相似文献
14.
本文利用我国部分台站地磁垂直分量日变幅的资料,采用局部地区日变场的分析方法,研究了地磁垂直分量日变幅在中国地区的空间分布特征.结果表明,在局部地区地磁日变场的研究中,考虑经度影响是必要的,本文所用方法是适宜的;结果还表明,垂直分量日变幅的空间分布呈现出明显的季节变化、逐月变化及逐日变化性.若粗略地把磁静日垂直分量日变幅极大值所处的纬度视为 Sq 高空电流体系的焦点所对应的纬度,则此焦点纬度夏季最高,冬季最低,春秋季居中,并显出明显的逐月及逐日变化性,在相邻的两个静日,焦点纬度的变化可达几度. 相似文献
15.
本文利用2014年9月到2017年8月全球高时空分辨率TEC数据对北半球四个经度带电离层中纬槽的发生率和槽极小位置的变化进行了统计研究.基于Kp指数,我们引入了一个包含地磁活动变化历史效应的地磁指数(Kp 9)来分析中纬槽位置变化与地磁活动水平的关系.通过与其他地磁活动指数的对比,发现槽极小纬度与Kp 9指数的相关性最好.此外,本文重点分析了中纬槽发生率及槽极小纬度的经度差异、季节变化、地方时变化以及与地磁活动强度等的关系.结果表明,中纬槽的发生率与经度关系不大,主要受到季节、地方时与地磁活动的影响.午夜中纬槽发生率在夏季较低,其随地方时的变化则呈现出负偏态分布的特点,在后半夜发生率更高,而地磁活动增强对中纬槽的发生具有明显的促进作用.对于槽极小纬度,其在四个经度带的分布差异不大,但月变化各不相同,其中-120°经度带呈单峰分布,在夏季槽极小纬度更高,而0°经度带夏季槽极小纬度更低.槽极小的位置显著依赖于地磁活动、地方时以及季节变化.一般说来,地磁活动越强,中纬槽纬度越低.中纬槽位置随地方时的变化有明显的季节差异,冬季昏侧槽极小纬度随地方时变化较快,弱地磁活动条件下22∶00 LT前即达到最低纬度,其后位置几乎保持不变,而两分季槽极小纬度从昏侧至午夜都在降低,夏季槽极小纬度从昏侧连续下降至03∶00 LT左右. 相似文献
16.
For a low-level geomagnetic satellite survey, for which the motion of the satellite converts spatial variation into temporal variation, the limit on accuracy may well be background temporal fluctuations. The sources of the temporal fluctuations are current systems external to the Earth and include currents induced in the Earth due to these sources. The internal sources consist primarily of two components, the main geomagnetic field with sources in the Earth's core and a crustal geomagnetic field.Power spectra of the vertical geomagnetic field internal component that would be observed by a spacecraft in circular orbit at various altitudes, due to satellite motion through the spatially varying geomagnetic field, are compared to power spectra of the natural temporal fluctuations of the geomagnetic field vertical component (natural noise) and to the power spectrum for typical fluxgate magnetometer instrument noise. The natural noise is shown to be greater than this typical instrument noise over the entire frequency range for which useful measurements of the geomagnetic field may be made, for all geomagnetic latitudes and all times. Thus there would be little benefit in reducing the instrument noise below the typical value of 10?4 gamma2 Hz?1 plus a 1/f component of 10 milligamma rms decade?1.For a given satellite altitude, there is a maximum frequency above which the natural noise is greater than the power spectrum of the crustal geomagnetic field vertical component. Below this maximum frequency, the situation is reversed. This maximum frequency depends on geomagnetic latitude (and to a lesser extent on time of day and season of year), being lower in the auroral zone than at lower latitudes. The maximum frequency is also lower at higher satellite altitudes. The maximum frequency determines the spatial resolution obtainable on a magnetic field map. The spatial resolution (for impulses) obtainable at low latitudes for a 100-km satellite altitude (possibly achievable by tethering a small satellite at this altitude to a space vehicle at a higher altitude) is 60 km, while at the auroral zone the obtainable spatial resolution is 100 km. At the higher satellite altitude of 300 km the obtainable spatial resolution is 230 km at low latitudes and 530 km at the auroral zone. At 500-km satellite altitude, the obtainable spatial resolution is 500 km at low latitudes, while maps cannot be made at all for the auroral zone unless the data are selected for “quiet” days.For the lower satellite altitudes, greater spatial resolution can be obtained than at higher altitudes. Furthermore since the crustal geomagnetic field power spectrum is larger at lower altitudes, the relative error due to the natural noise is less than for higher altitudes. 相似文献
17.
Wallace H. Campbell 《Pure and Applied Geophysics》1978,116(6):1143-1173
The Alaskar pipeline is a highly conducting anomaly extending 800 miles (1300 km) from about 62° to 69° geomagnetic latitude beneath the most active regions of the ionospheric electrojet current. The spectral behavior of the magnetic field from this current was analyzed using data from standard geomagnetic observatories to establish the predictable patterns of temporal and spatial changes for field pulsation periods between 5 min and 4 hr. Such behavior is presented in a series of tables, graphs and formulae. Using 2- and 3-layer models of the conducting earth, the induced electric fields associated with the geomagnetic changes were established. From the direct relationship of the current to the geomagnetic field variation patterns one can infer counterpart temporal and spatial characteristics of the pipeline current. The relationship of the field amplitudes to geomagnetic activity indices,A
p, and the established occurrence of various levels ofA
p over several solar cycles were employed to show that about half of the time the induced currents in the pipe would be under 1 A for the maximum response oscillatory periods near 1 hr. Such currents should be of minimal consequence in corrosion effects for even a section of the pipeline unprotected by sacrificial electrodes. Of greater interest was the result that the extreme surges of current should reach over one-hundred amperes in the pipeline during high activity. 相似文献
18.
O. M. Chugunova V. A. Pilipenko S. L. Shalimov M. Engebretson 《Geomagnetism and Aeronomy》2008,48(3):307-313
The variations in the daily average energy of geomagnetic pulsations and noise in the Pc3 (20–60 mHz) and Pc4 (10–19 mHz) frequency bands in the polar cap have been studied based on the data from P5 Antarctic station (corrected geomagnetic latitude ?87°) from November 1998 to November 1999. The daily average pulsation energy has been calculated using the method for detecting the wave packets, the spectral amplitude of which is higher than the threshold level, from the dynamic spectrum. A spectral analysis of the energy of pulsations and noise in the Pc3 and Pc4 bands, performed using the maximal entropy method, has revealed periodicities of 18 days in the local winter and 26, 13, and 7–9 days during the local summer. The simultaneous and coherent variations with periods of 26, 13, and 7–9 days in the solar wind velocity and IMF orientation indicate that the variations in the Pc3–4 wave energy in the polar cap at a sunlit ionosphere are mainly controlled by the parameters of the interplanetary medium. The variations in the Pc3–4 wave energy with a period of 18 days are observed only during the local winter and are supposedly related to the variations in the ionospheric conductivity modulated by planetary waves. 相似文献
19.
为探索地磁长期变化中地磁急变事件的识别方法,分析地磁急变的特征,本文基于多个地磁台站子夜均值数据,利用线性拟合方法计算了地磁场X,Y和Z三个分量的年变率,对近年来发生的地磁急变事件进行了识别和分析。结果显示:Y分量能对分析时段内已报道的地磁急变事件进行很好的识别,其中1999年的地磁急变事件,在我国区域内发生的时间可能为1998年,此外2017年可能存在一个新的地磁急变事件;Z分量年变率整体变化平缓,2001年和2013年前后发生两次显著的地磁年变率变化,并且分别早于2003年和2014年两次显著的地磁急变事件时间,这与下地幔的高电导率层对不同分量地磁信号从核幔边界传播至地表过程中的延迟作用有关;X分量年变率出现多次地磁急变事件特征,其变化与Dst指数年变率变化具有相关性,可利用其去除X分量年变率中存在的外部空间电流体系影响成分,更可靠地辅助Y分量对地磁急变事件进行识别。总体上,地磁子夜均值数据年变率的空间分布与基于第12代国际地磁参考场（IGRF12）模型计算的地磁数据年变率的空间分布所呈现的变化特征在总趋势上具有一致性,表明地磁台站子夜均值数据能够反映我国区域地球主磁场的变化特征,而分别由子夜均值数据和IGRF12模型计算的2003年Y分量年变率空间分布均存在的显著局部特征,可能与地磁急变事件的区域特征有关。 相似文献