共查询到17条相似文献，搜索用时 156 毫秒
1.
用国际参考地磁场模型(IGRF)分析了地磁场能量在地球内部的分布及其长期变化.结果表明,从1900年到2005年,地核以外地磁场总能量由6.818×1018J减少到6.594×1018J,减小了3.3%,地表以外地磁场总能量由8.658×101J减小到.63×101J,减小了11.4%.分析地球内部不同圈层地磁场能量的变化表明,地壳(A层)、上地幔(B层)、转换带(C层)、下地幔D′层的地磁场总能量在减小,但是下地幔"层的地磁场总能量却在快速增加.磁能密度随时间的变化更清楚地显示出磁能增加和减小的分界面在r=3840km处.上述结果表明,地核和地表以外地磁场总能量在趋势性减小的同时,也在进行重新分配.进一步分析表明,下地幔D"层磁能快速增长,主要是由高阶磁多极子的增强引起的.在地磁场倒转前,偶极矩减小而多极性相对增强在能量分布上的表现就是磁能向下地幔底部(特别是D"层)集中. 相似文献
2.
为了研究中国境内各阶非偶极子(ND)磁场,通过最新的地磁场模型CALS10K.1b计算了10000 BC—AD 1990年ND磁场在中国境内的时空及能量变化;22,23和24极子磁场零值线主要呈现出从我国中北部向东南部移动,从北部向东部移动,以及从东南部向西北部移动的趋势;除了26极子磁场,其余ND磁场在1500年以后均有“翘尾”现象,其所占主磁场的比值在10000 BC—AD 1500年呈震荡变化,从1500年开始快速上升;除了22极子磁场,其它各阶ND磁场能量随时间变化的趋势基本一致. 在5650 BC年左右,各阶ND磁场能量值均出现高值并随阶数的增大而衰减,反映了在该时间点通过地核发电机产生的磁场能量随径向距离而近似线性衰减,地磁场能量主要源自地球液态外核. 将CALS10K.1b模型结果与IGRF11模型对比后,得出CALS10K.1b模型所计算的ND磁场及能量值较为可靠,而两者差异主要源于数据和建模方法的不同. 相似文献
3.
为了综合反映地球表面行星尺度磁异常的展布面积、磁场极值以及磁场分布特征等多种因素及其与磁能的关系，本文用穿过各异常区的“无符号磁通量”为特征参数来表征磁异常区强度.用第八代国际参考地磁场模型(IGRF)，分析了1900年到2000年全球最大的5个磁异常区的长期变化，结果表明，在一百年中，南大西洋(SAT)、大洋洲(AUS)和非洲(AF)3个异常区的磁通量均增加了200MWb以上，欧亚异常(EA)磁通量增加幅度稍小(157MWb)，上述4个异常区磁通量增幅为30%-60%，而北美异常(NAM)的磁通量则减小了50MWb.各异常区面积虽有变化，但最大变化仅为%左右.对磁异常区的西向漂移研究表明，地球表面和核幔界面的西漂明显存在差异：地表磁场有持续而稳定的西向漂移，全球平均西漂速度为0.2°/a；但核幔界面磁场的西向漂移速度要小得多，最大不超过0.1°/a.形成这种差异的原因可能是组成地磁场的不同球谐分量有不同的漂移速度；地表磁场的西漂主要决定于占优势的低阶分量，而核幔界面的西漂则受到高阶分量的重大影响.本文指出，在把地表西漂值用作地核磁流体运动速度的典型值时必须十分谨慎. 相似文献
4.
根据历史地磁场模型GUFM1、第10代国际参考地磁场（IGRF10）模型和日长资料,采用小波变换方法,分析了地磁场磁矩、能量、西向漂移等参数的长期变化和日长十年尺度变化的周期分量及其时变特征.结果表明,1800～2005年期间,偶极子磁场长期变化有82年和48年准周期分量,它们与日长变化的周期没有直接关系.非偶极子磁场参数的长期变化与日长变化有66年和32年准周期分量,66年准周期比32年准周期强.在66年准周期分量,西向漂移比日长变化超前8.8年,非偶极子磁场能量比日长变化滞后15.6年.日长十年尺度波动和地磁场长期变化的起源不存在因果关系. 相似文献
5.
地球主磁场的能量密度谱及其长期变化 总被引：6，自引：3，他引：6
根据BJ地磁场模型和第8代国际地磁参考场(IGRF)模型，计算并分折了1690～2000年期间地球表面主磁场和分量的能量密度谱及其长期变化。结果表明1690～2000年期间主磁场的能量密度谱一直在减小，其主要原因是由于偶板子磁场的衰减产生的，而非偶板子磁场的能量密度谱在1690～1780年期间减小，1780～1890年增大，1890年以后快速增大。在地磁场总能谱的变化中，Z分量的贡献起主要作用。能量密度随谐波阶数的变化在半对数坐标中近似线性，非偶板子场的等效磁源深度位于核幔边界附近，n＝1，2谐波项的等效磁源位于地球内核边缘，其位置随时间变化。1780和1890年前后是地磁场变化的转折时期。能量密度谱的长期变化存在大约60a的周期规律。 相似文献
6.
1.前言地球基本磁场随时、空有一个周期性的、长期缓慢的变化。一般认为,这种变化来源于地核内部或核幔边界,因此,利用地磁场的这种长期变化的规律,可以研究地球内部物质的 相似文献
7.
虚地磁极（VGP）的角离散携带着地磁场低阶非轴向偶极子分量空间变化的重要信息．重申地球主磁场定解问题的适定性，指出McFadden等模型G存在重复计入轴向偶极子分量的内在矛盾；作为模型G基础的VGP角离散的偶极族-四极族分解仅具有数据拟合意义．证明，如果地磁场的非轴向偶极子分量相对轴向偶极子分量为小量，那么VGP角离散的纬度变化主要由轴向偶极子Gauss系数约化的低阶Gauss系数的平方和决定．因此作出估计，在过去5Ma中，赤道偶极子和赤道四极子的Gauss系数的幅度大致相当，约为轴向偶极子Gauss系数的10％． 相似文献
8.
1900~2000年的IGRF(国际地磁参考场)资料使研究20世纪中地磁场的变化规律成为可能,在20世纪中,即使从19世纪起,地球偶极子磁场发生了较大的变化,偶极矩一直保持衰减的势头,地心轴的所有3个分量都是减小的.地磁南极的位置变化在1930年左右发生大的转折,1960年起向西和向南快速移动,偶极子轴在纬度方面变化只有1°左右,经度变化在3°左右,离磁极倒转的条件差得远. 相似文献
9.
地球内部磁场的变化时间从数月到数十亿年不等。地磁场是由液态外地核对流产生的,从而受到从地核到地幔底部热流的影响。地磁场的变化在很大程度上被认为是随机的,但是它的长期变化可能与地幔对流过程中的热流变化有关。在过去的500Ma中,古地磁行为与地表过程的联系在始于约180Ma前的中生代中晚期尤为显著。地球发电机模拟表明,侏罗纪中期到白垩纪中期之间发生了磁极快速反转时期到持久稳定时期的转变,这或许是球对称的或者赤道方向的核幔边界热流的减少所触发的。该热流的减少可能与核幔边界处地幔柱顶冠活动的减弱有关,或者与真极移有关,亦或与二者同时有关。 相似文献
10.
在国际参考地磁场（IGRF）模型中，高阶球谐系数比低阶系数小得多，所以高阶项对主磁场的贡献常被忽略不计. 但是，高阶项对主磁场的长期变化却有重大影响. 本文根据第八代IGRF模型，分析了IGRF 1945～1955中高阶球谐系数的异常特征对长期变化的影响，然后用修正IGRF模型估计并改正了这些影响. IGRF高阶项随深度增加而迅速增大，所以高阶系数的误差对深部磁场位形和磁场能量的计算有不可忽视的影响，对核幔界面流动状态的推断和地核半径的地磁估计有更为重大的影响. 相似文献
11.
Summary The harmonically variable magnetic field, generated by a tangential magnetic dipole (TMD), located eccentrically at the surface of the Earth's core, is investigated for various periods of time variations and for a three-layer conductivity model of the Earth. Numerical computations have shown that the field is inductively damped for variation periods of less than 500 years as compared to the field of a static TMD. It is proved that the field appropriate to the TMD, has a more complicated distribution of the Earth's surface than the field of a radial magnetic dipole. Comparison with maps of the non-dipole part of the geomagnetic field shows that the TMD is not as suitable for interpreting the observed non-dipole field and its variations as the eccentric radial magnetic dipole. 相似文献
12.
13.
The works on paleomagnetic observations of the dipole geomagnetic field, its variations, and reversals in the last 3.5 billion years have been reviewed. It was noted that characteristic field variations are related to the evolution of the convection processes in the liquid core due to the effect of magnetic convection and solid core growth. Works on the geochemistry and energy budget of the Earth’s core, the effect of the solid core on convection and the generation of the magnetic field, dynamo models are also considered. We consider how core growth affects the magnetic dipole generation and variations, as well as the possibility of magnetic field generation up to the appearance of the solid core. We also pay attention to the fact that not only the magnetic field but also its configuration and time variations, which are caused by the convection evolution in the core on geological timescales, are important factors for the biosphere. 相似文献
14.
Summary Theoretical formulae are derived for computing a variable magnetic field, excited by a harmonically oscillating radial magnetic dipole (RMD), located eccentrically at the surface of the Earth's core. By numerical computations, using a three-layered conductivity model of the Earth, it is proved that the field due to this source, computed for the surface of the Earth, is relatively weak in comparison to the field of a stationary magnetic dipole, provided the period of the changes is less than 500 years. The zone of influence of the RMD at the Earth's surface is also determined and on its basis a number of conclusions were drawn with respect to representing the non-dipole part of the geomagnetic field by means of the RMD system in the Earth's core.Dedicated to RNDr. Jan Pícha, CSc., on his 60th Birthday 相似文献
15.
J. A. Jacobs 《Surveys in Geophysics》1998,19(2):139-187
The Earth's main magnetic field can be approximated by an axial, geocentric dipole. The remaining non-dipole field is much smaller and is a regional rather than a global feature – quite large changes can occur in a few ka. This review is concerned with changes in the dipole component of the geomagnetic field, and one of the problems is in separating the non-dipole from the dipole contributions to the field. Unlike the many determinations of the direction of the Earth's magnetic field in the past (which have led to fundamental contributions to our understanding of plate tectonics and shown that the field can on occasion reverse its polarity), estimates of the intensity of the field are comparatively few, especially before the Holocene. This is mainly the result of experimental difficulties in obtaining reliable measurements of the field. These problems are discussed in some detail and are followed by a short account of archaeomagnetic intensities and results from Hawaii where many of the first determinations were obtained. Measurements for the last 100 ka from both lavas and lacustrine and oceanic sediments are reviewed and results from different areas compared. An asymmetric saw-tooth pattern has been observed in some of the records over the last few Ma, and this rather controversial question is discussed. Finally an account is given of the far more limited data on palaeointensities in earlier times.A short discussion is given of the interpretation of coherent short wavelength variations which are observed in many marine magnetic profiles. Although short reversals of the field may be responsible for some of these tiny wiggles, it is more likely that in general they are the result of changes in the strength of the Earth's magnetic field. 相似文献
16.
17.
A. E. Levitin L. I. Gromova S. V. Gromov L. A. Dremukhina 《Geomagnetism and Aeronomy》2014,54(3):292-299
A new method for determining geomagnetic activity based on calculation of the hourly amplitudes of geomagnetic field variations at ground-based observatories has been developed. Observations performed in 2009, when unusually low solar and geomagnetic activity was registered, were used as a reference level. The described method was used to estimate the energy of local geomagnetic activity; such energy is estimated for observatories in the Earth’s Northern and Southern hemispheres, and a total estimation is made for both hemispheres and for the entire Earth’s surface during large magnetic storms. These are used to compare characteristics of magnetic storm intensity based on the classical Kp and Dst indices and calculated energy estimate. 相似文献