水介质对水下目标体磁场的影响

根据扬子江航道上一系列磁测及验证结果,指出在不同介质中的相似磁性物体所引起的磁场强度会产生一定的变化,实例说明：这一现象可能对磁法勘查带来的影响.文章没有对不同介质中磁性体磁场的变化机制进行讨论.     

低轨磁测卫星干扰磁场标定方法研究

为了提高空间磁场探测精度,磁测卫星一般将磁强计安装在长伸杆的顶端,同时通过整星磁洁净控制,来减小磁强计安装位置的磁场干扰量.针对低轨磁测卫星的特点,提出零磁场环境下卫星极弱干扰磁场的高精度测量方法,模拟在轨地磁场环境下卫星感应磁场的标定方法,以及磁力矩器剩磁不确定量的处理方法.通过以上方法对卫星本体产生的干扰磁场实施严格的标定和数据修正,可有效减小其影响,极大提升空间磁场探测精度.该方法已应用于电磁监测卫星,将整星的磁场干扰不确定量降低一个量级,达到优于0.3 nT的水平.     

磁测找油方法及其在陕北油气勘探中的应用

二十多年来,磁测找油方法作为非地震油气物探方法中的一种,在陕北油田进行了大量的试验及研究工作.为了系统归纳磁测找油方法研究进展及探讨其在陕北油气勘探中的应用效果,本文阐述了油气藏上方近地表微磁异常的形成机理以及磁性矿物的形成机制的研究进展,总结了由于地下油气藏的存在而引起的微磁异常的一般特征,分析了陕北吴堡-旦八地区已有油井及干井的分布特征与高磁剩余异常特征间的关系.结果表明,油气藏上方岩石中广泛存在的磁学-地球化学-矿物学异常与烃类微渗漏作用之间的相互关系基本可以成立,烃渗漏可以通过改变油气藏上方空间氧化还原条件等造成磁性变化从而在近地表产生磁异常变化,而这些磁异常在经过数据处理之后,可以提供微磁异常与油气藏之间高度的相关性.陕北吴堡-旦八地区高磁剩余异常与油井具有一定的相关性,高频、低幅度、高值异常带以及高值环带包围低值区块的环带异常与油气藏有较好的对应关系.虽然目前还不可能研究出一种可以完全消除或大部分压制地面上各种人文干扰产生磁场的方法技术,但是在开展高精度磁测工作时,尽量压制各种与油气藏无关的干扰磁异常,并且做好物性测定和样品分析,磁测找油方法仍不失为一种经济、快速、有效的方法.     

地磁台站建设中磁测异常现象分析

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。     

卫星磁洁净的控制和测量

本文叙述卫星磁洁净的重要性、空间磁场的分布、卫星磁性的要求、卫星磁矩的来源、卫星的磁设计和控制、卫星和它的部件的磁矩的测量方法、内容、过程、装置和一些部件的测量结果.卫星磁矩来自三个方面,它们是永磁铁,软磁材料和杂散磁场(电流产生的磁场).磁性设计包括材料选择、器件的测试、电子线路的布置和元件的安排等.     

一种磁张量探测系统载体的磁张量补偿方法

针对磁张量系统载体产生的磁张量值对系统测量精度产生很大影响的问题,以及现有磁补偿模型存在非线性、分体式和参数多的问题,提出一种磁张量系统载体的一体化线性磁张量补偿方法.分析了载体硬磁材料产生固有磁张量值和软磁材料产生感应磁张量值的微观机理,并推导了相应的数学表达式,结合固有磁场影响和感应磁场影响建立了载体磁张量补偿模型.模型中含有20个载体磁张量补偿系数,对模型求解得到补偿系数,结合三分量磁场测量值即可达到对载体磁张量的补偿.实测实验表明,磁张量补偿方法计算得到的载体磁张量值与载体实际产生的磁张量值仅差32nT/m,可以有效完成对磁张量系统的载体磁张量补偿.     

加热环境对人工合成磁赤铁矿热磁行为的影响

热磁测量,包括高温磁化率和高温磁化强度测量,是根据热磁曲线转折点的温度(居里点、尼尔点或相变点)鉴定样品中磁性矿物种类的有效方法.本文选取两个人工合成磁赤铁矿样品,利用四种热磁测量仪器分析不同的条件下测得的热磁曲线.依据样品与空气接触程度,将测量环境设为开放、封闭、封闭(通入氩气或氮气)三类.结果表明:热磁测量环境的开放程度对居里点和曲线可逆程度产生极大的影响.封闭环境下测得的居里点较开放环境下的低,分别对应磁铁矿和磁赤铁矿;开放系统的热磁曲线不可逆程度高于封闭系统.造成这些差异的原因是氧化还原条件的不同.本文的磁赤铁矿样品在封闭的条件下,加热至250 ℃左右开始转化为磁铁矿,因此无法通过居里点被正确识别;在开放的氧化环境下,加热的最终产物为赤铁矿,能够测得正确的居里点.本实验结果启发人们:在不同的加热环境下,磁性矿物可能表现出不同的热磁行为,根据单一的热磁曲线,很容易对样品中磁性矿物的种类造成误判.全面对比不同条件下的测量结果,才能够得出更为准确的结果.     

涉县地磁台地磁观测室建设材料磁性检测

涉县地磁基准台地磁观测室在建设过程中严格按照观测规范要求施工,利用GSM-19T磁力仪,对建筑材料磁性进行严格检测和筛选,并对地磁房建设前后磁场梯度进行检测,对比可以发现磁房场地磁场梯度是否符合规范要求。此次涉县地磁房建设过程中各种建筑材料的磁性检测工作,可以为其他台站磁台建设提供参考。     

一阶反转曲线（FORC）图的原理及应用实例

自然样品中的磁性矿物携带着丰富的环境演化信息．然而在一般情况下,自然样品的磁性是其含有的诸多磁性矿物的综合反映．为了分离这些磁信息,近年来发展了一种新的岩石磁学方法：一阶反转曲线（FORC）图．该方法不但可以确定磁性矿物矫顽力的分布以及磁性矿物颗粒之间磁相互作用的强弱,而且还可以帮助区分磁性矿物的种类和磁畴状态．本文首先详细介绍该方法的基本原理和其物理意义,在此基础上,给出了一个应用FORC图确定含铝的钛磁铁矿玄武岩样品中磁性矿物在加热过程发生转变的研究实例．在两个温度下的FORC图密度分布差的结果表明,这种新方法可以灵敏地检测样品中微弱的磁性矿物改变,因此在岩石磁学、环境磁学和古地磁学研究中具有很好的应用前景．     

航磁弱异常区磁场水平调整——以黔东地区为例

航磁磁场水平调整是压制非地质因素对磁场的干扰,还原磁场本来面貌的重要手段,传统方法主要为切割线调平和微调平,但在弱磁场区实测磁场面貌不清晰,干扰异常影响突出,使用常规磁场水平调整方法难以达到理想的处理效果.本文针对黔东地区航磁弱异常,在介绍弱磁场成因、磁场水平误差表现形式的基础上,对该地区磁场水平进行了调整.为获得较好的磁场水平调整效果,使用了弱磁场区水平调整方法,并针对弱磁场区高压线等干扰异常明显的特点,利用该方法对区内高压线干扰异常进行处理,处理后的磁场趋势更合理,磁场面貌更清晰,突出了微弱局部异常,更好地满足后续数据转换处理和地质解释的需要.     

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.     

The first magnetic chart

Almost 300 years to the day since Edmond Halley's first magnetic chart, the RAS held a Discussion Meeting to commemorate this achievement and to consider Halley's work in navigation and geophysics. David Barraclough and Toby Clark report on the "300th anniversary of the first magnetic chart: Edmond Halley's work in geophysics and navigation".