基于重磁泊松定理的磁化方向估计及应用：以相山铀矿田为例

磁化方向的确定对磁异常处理、反演及解释方面有着重要的参考价值.然而,目前常用的磁化方向估计方法易受计算窗口尺度、化极或叠加异常等影响.为此,本文从重磁泊松定理出发,推导出了磁化强度、磁异常一阶导数及重力位三阶导数的关系式,并在此基础上构建出了可反演磁化强度三分量的线性方程组,进而获得了场源的磁化倾角与偏角.模型试验表明,本文方法能够在多场源的叠加重、磁异常上,有效地反演出各场源的磁化方向,但噪声会在一定程度上降低反演精度,尤其对小规模场源的磁化方向影响较明显.将本方法应用于江西相山铀矿田重磁资料之中,获得了10个测算点的磁化方向,推断了这些测算点位置上重磁同源体的岩石类型,结果表明了研究区内碎斑熔岩具有强剩磁特征,而流纹英安岩则为顺磁性物质,且认为碎斑熔岩之下广泛分布着流纹英安岩,这对该地区组间界面部位铀矿找矿具有重要的指导意义.     

剩磁影响下磁性体磁化方向估计的一种简单算法

磁测资料处理解释通常需要已知场源的磁化方向信息.在剩磁影响下,总磁化方向与感应磁化方向并不一致,这使得处理解释变得复杂.本文研究提出从近等轴状磁总场异常估计磁化方向的偶极源互相关法,即用磁偶极源的理论磁异常与实测磁异常作互相关,用一系列递变的偶极源位置和磁化方向做试错,取互相关最大化对应的磁化方向作为估计结果.理论数据试验和中国西北某金属矿勘探区航磁资料试验表明本文方法能从近等轴状磁异常有效估计出总磁化方向.     

斜磁化磁异常处理方法分析

受斜磁化的影响,磁异常特征复杂、不便于解释.强剩磁的存在、低纬度化极的困难等问题常常迫使人们直接针对斜磁化磁异常开展处理与反演.为了减小斜磁化的影响,磁异常总梯度模、分量模、磁异常梯度张量等处理方法得到广泛应用.本文基于理论分析,结合模型实验,分析现有斜磁化磁异常处理方法的优缺点,指出磁异常总梯度模、分量模、磁异常梯度张量等处理方法可能引起错误的地质解释,而采用适当的化极计算则可以明显改善解释效果.     

强剩磁强退磁条件下的二维井中磁测反演

强剩磁、强退磁改变了总磁化强度的大小和方向,给磁测资料解释带来困难.为此,本文利用二维井中磁测数据反演磁化强度矢量的二维分布.首先利用井中磁测的磁异常模量反演磁化强度大小的分布.然后,在已知磁化强度大小分布的前提下,拟合磁场分量,反演磁化强度方向的分布.其中,磁化强度大小和方向均用共轭梯度法求解,并通过预优矩阵改善磁化强度大小的反演效果.理论模拟说明,该方法能准确获得磁化强度矢量分布.磁化强度矢量反演结果包括感磁、剩磁及退磁的影响,这为研究强剩磁、高磁化率矿床提供了一种有效方法.     

磁化强度矢量反演新方法及其在卡拉塔格铜多金属矿床找矿中的应用

磁异常的反演是地球物理勘探的重要手段,三维磁化率反演是磁异常定量解释中的一种重要方法.由于剩磁的存在使得磁化方向与地磁场方向产生偏差,从而影响了磁异常反演与解释的精度.本文基于磁异常模量反演和磁化强度矢量反演方法得到了一种新的磁化强度矢量反演方法.与以往的磁化强度矢量反演方法相比,该方法以磁异常模量反演得到的磁化率模型为约束,采用Lp范数正则化方法求解,提高了磁化强度矢量反演的精度和效率.本文通过模拟试验的反演计算,验证了这种磁化强度矢量反演方法的有效性.最后,将本文方法应用于新疆东天山卡拉塔格地区航磁数据的解释,获得了地下空间不同磁性差异的磁性体的空间分布特征,为进一步分析研究区隐伏矿床提供了重要信息.     

基于欧拉反褶积方法的航磁三分量应用研究

在中国北部某地区首次开展了航磁三分量矢量飞行测量.本次测量是国内第一次直接测量航磁异常三分量Z_a、H_(ax)、H_(ay)数据,即文中提到的垂直分量V、北分量N、东分量E.由于三分量磁测数据具有矢量空间性,因而凭借其全空间矢量,在反演过程中可以更直接地发挥指向性作用.更为丰富的测量资料参与反演,所得到的最终结果为构造解释提供了更有力的约束,从而有助于减少地质解释过程中的多解性,提升解释结果的可靠性.本文以模型试验为切入点,首先进行三个分量各自的欧拉反褶积处理模型试验,以模型试验结果总结了不同的分量经反演后各自对理论模型边界刻画的特点.而后依据以上特点,将三个分量各自的反演结果进行叠加.与总场的反演结果相比,三个分量反演的叠加结果改善了模型体边界的识别效果,获得了更为准确的模型体位置信息.在总结了模型试验相关规律的基础之上,按照类似步骤分别对实测航磁三分量数据进行了欧拉反褶积处理,再将三个分量实测数据各自的反演结果进行叠加,以叠加后的结果进行构造解释.利用不同分量各自的反演特点,综合发挥多分量的资料优势,最终以三分量反演的叠加结果为依据,有效地识别了区内断裂,更加准确地刻画出断裂的形迹位置,揭示了不同性质断裂的世代关系,显示了良好的应用效果.     

数据空间磁异常模量三维反演

强剩磁的存在通常导致了总磁化强度方向未知,进而影响了磁异常的反演和解释.磁异常模量是一种受磁化方向影响小的转换量,可以在强剩磁条件下通过反演三维磁化强度大小分布来推测场源分布状态.我们提出了一种数据空间磁异常模量反演算法来减少剩磁的影响.与标准的模型空间L2范数正则化反演方法相比,我们的方法有两个优点:一是无需搜索正则化参数(需要反复求解非线性反演问题),因而可以减少计算时间;二是反演结果更加聚焦,深度分辨率更高,我们对此进行了原因分析.通过模型和实测数据测试证明了该算法的有效性和更好的反演效果.     

基于方向tilt-Euler的三维磁数据快速反演

三维磁异常快速反演是磁法勘探进行地质解释的一项重要内容.本文在方向tilt梯度基础上进行导数处理,并进行合理改进,得到了6个改进的方向tilt梯度导数,丰富了不同方向上的磁异常信息.对常规欧拉反褶积方程进行三个方向求导,所构成的方程组与6个改进的方向tilt梯度导数进行结合,从而构建出了两个基于方向tilt梯度导数的快速反演方程组(方向tilt-Euler法),用于反演场源的位置参数.另外,将三个方向导数下的欧拉反褶积进行平方和及均方根处理,得到了场源构造指数的求解公式.单一模型试验表明,6个改进的方向tilt梯度导数异常基本不受磁化方向影响,可从不同方向上反映磁异常信息,方向tilt-Euler能够准确地反演出场源的位置及构造指数.叠加模型试验证实了方向tilt-Euler法相对于tilt-Euler法,具有反演解聚集度更强、连续性更好、反演准确度更高、受噪声影响更小及无虚假反演解等优点.将本文方法应用于内蒙古塔木素航磁资料处理中,获得了丰富的地下磁源分布信息,为了解该地区隐伏断裂构造及岩体分布等提供了有效依据.     

吐鲁番中南部地区航磁异常特征及其地质意义

为了深入研究吐鲁番中南部地区航磁异常特征及其地质意义,本文基于1:50000航空磁力ΔT总场异常数据计算了航磁化极异常,并对航磁化极异常数据利用正则化滤波方法进行了异常的分解、利用罗森巴赫Ⅱ式进行了垂向二阶导数异常的换算,获取了吐鲁番中南部地区区域磁力异常、局部磁力异常及垂向二阶导数异常.结合已有的地质及地球物理研究成果,对航磁异常特征进行了深入分析,并就磁力异常与地表地质信息之间的关系进行了深入研究,探讨了本区断裂分布、岩浆岩分布及磁性特征.研究结果表明,研究区太古界总体表现为较强磁性,元古界、古生界、中生界及新生界总体表现为弱磁性.研究区构造复杂,断裂构造特征具有明显的分区性.研究区岩浆活动明显受构造控制,岩体长轴与构造走向一致.研究区中性岩表现为弱磁性,而酸性岩则大致以独峰山—梧桐沟一线为界表现为北弱南强的磁性特征.     

应用磁视散度及磁源重力异常确定低磁纬度地区磁性体分布-以哥伦比亚普图马约盆地为例

低磁纬度地区受斜磁化的影响,用常规方法很难准确确定磁性体的平面分布特征.为了研究位于低磁纬度地区普图马约盆地的磁性体分布特征,本文根据场的散度原理,假定磁△T异常为具有一定方向的矢量场,其方向与磁化方向一致,导出了磁△T异常视散度的计算方法;根据磁位与引力位的关系,在频率域中通过磁△T异常求取了磁源重力异常,并尝试利用拉普拉斯方程计算磁源重力异常垂向二阶导数.本文设计理论模型讨论了磁△T异常视散度、磁源重力异常垂向二阶导数的特征与磁性体平面分布特征的关系,证明了上述方法的有效性.进而利用上述方法推测了普图马约盆地磁性体的平面分布特征,结果表明:应用磁视散度及磁源重力异常确定的普图马约盆地磁性体分布与实际地质特征吻合较好,取得的成果对普图马约盆地相关地质研究及对低磁纬度地区的磁性体的确定有一定的参考意义.     

磁屏蔽室内磁性样品所产生干扰磁场的探讨

磁屏蔽室内岩石和各种沉积物样品所受的地磁场影响可以被有效地压制,然而磁性样品本身也会产生次级干扰磁场.本文通过理论模拟计算,定量评估了这种次级干扰磁场的影响.结果发现无论是单个还是聚集在一起的磁性样品,其产生的干扰磁场一般都低于磁屏蔽室的本底值(～300 nT).因此,弱磁性样品的相互影响可以忽略不计.这为进一步理解古...     

Extraterrestrial magnetic minerals

Thermomagnetic and microprobe analyses are carried out and a set of magnetic characteristics are measured for 25 meteorites and 3 tektites from the collections of the Vernadsky Geological Museum of the Russian Academy of Sciences and Museum of Natural History of the North-East Interdisciplinary Science Research Institute, Far Eastern Branch of the Russian Academy of Sciences. It is found that, notwithstanding their type, all the meteorites contain the same magnetic minerals and only differ by concentrations of these minerals. Kamacite with less than 10% nickel is the main magnetic mineral in the studied samples. Pure iron, taenite, and schreibersite are less frequent; nickel, various iron spinels, Fe-Al alloys, etc., are very rare. These minerals are normally absent in the crusts of the Earth and other planets. The studied meteorites are more likely parts of the cores and lower mantles of the meteoritic parent bodies (the planets). Uniformity in the magnetic properties of the meteorites and the types of their thermomagnetic (MT) curves is violated by secondary alterations of the meteorites in the terrestrial environment. The sediments demonstrate the same monotony as the meteorites: kamacite is likely the only extraterrestrial magnetic mineral, which is abundant in sediments and associated with cosmic dust. The compositional similarity of kamacite in iron meteorites and in cosmic dust is due to their common source; the degree of fragmentation of the material of the parent body is the only difference.     

Lunar magnetic variations

Displayed daygraphs of magnetic observatory hourly mean values and of lunar magnetic variations reconstructed from spherical harmonic coefficients are used to illustrate the difficulties that arise in separating lunar magnetic effects from those associated with the 27 day recurrence tendency in magnetic activity.     

Small-scale magnetic buoyancy and magnetic pumping effects in a turbulent convection

We determine the nonlinear drift velocities of the mean magnetic field and nonlinear turbulent magnetic diffusion in a turbulent convection. We show that the nonlinear drift velocities are caused by three kinds of the inhomogeneities; i.e., inhomogeneous turbulence, the nonuniform fluid density and the nonuniform turbulent heat flux. The inhomogeneous turbulence results in the well-known turbulent diamagnetic and paramagnetic velocities. The nonlinear drift velocities of the mean magnetic field cause the small-scale magnetic buoyancy and magnetic pumping effects in the turbulent convection. These phenomena are different from the large-scale magnetic buoyancy and magnetic pumping effects which are due to the effect of the mean magnetic field on the large-scale density stratified fluid flow. The small-scale magnetic buoyancy and magnetic pumping can be stronger than these large-scale effects when the mean magnetic field is smaller than the equipartition field. We discuss the small-scale magnetic buoyancy and magnetic pumping effects in the context of the solar and stellar turbulent convection. We demonstrate also that the nonlinear turbulent magnetic diffusion in the turbulent convection is anisotropic even for a weak mean magnetic field. In particular, it is enhanced in the radial direction. The magnetic fluctuations due to the small-scale dynamo increase the turbulent magnetic diffusion of the toroidal component of the mean magnetic field, while they do not affect the turbulent magnetic diffusion of the poloidal field.     

Determination of magnetic cloud parameters and prediction of magnetic storm intensity

A program for identifying magnetic clouds in patrol satellite data, which recorded the interplanetary medium parameters near the magnetosphere, has been developed based on the cloud model in the form of a force-free cylindrical flux tube. The program makes it possible to also determine the entire magnetic field distribution in a cloud that approaches the Earth, using the initial satellite measurements. For this purpose, a model cloud (which has the maximal correlation coefficient with an analyzed cloud with respect to three magnetic field vector components and minimal rms deviations of the magnetic field and velocity components) is selected from the preliminarily created database including 2 million model clouds. The obtained magnetic field distribution in a cloud will make it possible to predict the intensity of a magnetic storm that this cloud will cause.     

Mesozoic magnetic lineations and the magnetic quiet zone off northwest Africa

An extensive compilation of recently acquired geophysical reconnaissance data has allowed the Mesozoic magnetic lineations (The Eastern Keathley sequence) to be identified and mapped in detail for the area off northwest Africa lying between Madeira and the Cape Verde Islands. These anomalies were generated as one limb of a symmetric spreading center (Paleo Mid-Atlantic Ridge) from about 107 to 153 m.y.B.P. Offsets in the lineation pattern serve to identify fracture zone traces whose trends are approximately east-west. The seaward boundary of the marginal quiet zone does not precisely define an isochron due to the presence of a variable width transition zone of intermediate amplitude magnetic anomalies. Crust underlying the marginal quiet zone was generated, at least in part, during the Jurassic, Graham normal polarity epoch. The quiet zone boundary is not offset significantly on opposite sides of the Canaries lineament as previously suggested. A possible counterpart of the U.S. east coast magnetic anomaly is observed in some areas near the shelf/slope break of Spanish Sahara and Mauritania. The presence of relatively high-amplitude (but not-correlatable) magnetic anomalies seaward of the Mesozoic sequence and presumably generated during the Cretaceous, Mercanton normal polarity epoch remains a paradox.     

日面方位磁场扰动和行星际磁场螺旋结构

文采用球坐标下2.5维理想MHD模型,对日球子午面内方位磁场扰动的传播进行数值模拟,重点分析它对行星际磁场螺旋角的影响. 本文认为,观测到的行星际磁场螺旋角大于Parker模型的预言值,是太阳表面不断向行星际发出同向方位磁场扰动的结果;太阳较差自转在太阳内部产生的方位磁场为这类扰动提供了源头. 模拟结果表明,采用持续时间等于周期的十分之一、扰动幅度为103nT量级的正向方位磁场扰动,就可使1 AU处行星际磁场的螺旋角增加2°左右,与有关观测结果相符. 模拟结果还表明,上述方位磁场扰动对日球子午面内的太阳风特性和磁场位形的影响基本上可以忽略.     

Solar polar magnetic field

The solar polar magnetic field has attracted the attention of researchers since the polar magnetic field reversal was revealed in the middle of the last century (Babcock and Livingston, 1958). The polar magnetic field has regularly reversed because the magnetic flux is transported from the sunspot formation zone owing to differential rotation, meridional circulation, and turbulent diffusion. However, modeling of these processes leads to ambiguous conclusions, as a result of which it is sometimes unclear whether a transport model is actual. Thus, according to the last Hinode data, the problem of a standard transport model (Shiota et al., 2012) consists in that a decrease in the polar magnetic flux in the Southern Hemisphere lags behind such a decrease in the flux in the Northern Hemisphere (from 2008 to June 2012). On the other hand, Svalgaard and Kamide (2012) consider that the asymmetry in the sign reversal simply results from the asymmetry in the emerging flux in the sunspot formation region. A detailed study of the polar magnetic flux evolution according to the Solar Dynamics Observatory (SDO) data for May 2010–December 2012 is illustrated in the present work. Helioseismic & Magnetic Imager (HMI) magnetic data in the form of a magnetic field component along the line of sight (the time resolution is 720 s) are used here. The magnetic fluxes in sunspot formation regions and at high latitudes have been compared.     

An overview of the external magnetic field with regard to magnetic surveys

Surveys in Geophysics -     

太阳黑子磁场极性指数时间序列

本文根据苏黎世天文台太阳黑子11年周期资料和太阳黑子磁场磁性变化周期特征,构建了太阳黑子磁场磁性指数IM(Magnetic Index)时间序列,用IM(i)表示.为了便于采用数学方法研究太阳黑子磁场磁性指数变化与诸多地球物理现象之间的联系,本文给出了1749～2007年月平均太阳黑子磁场磁性指数时间序列数据.