基于Weimer模型的高纬地磁扰动预测

地磁扰动是空间天气中的重要现象,对地基技术系统具有重要的影响.准确预报地磁扰动可以有效避免重大灾害发生.本文基于Weimer电势和磁势模型发展了高纬地区地磁扰动的模拟方法,并与地面台站观测数据进行了比较.地表磁场扰动主要受电离层电流系统的影响,利用Weimer模式计算出电离层等效电流分布后,基于毕奥-萨伐尔定律推导了地磁扰动三分量与电流的关系,最终计算出地磁扰动量.模型的输入参数为太阳风速度、太阳风密度、行星际磁场和磁偶极倾角.模型计算结果与不同纬度和经度的地磁台站观测结果对比表明本文的计算方法能有效地模拟地磁暴期间地磁扰动特征.本文结果对今后发展高纬地区地磁场预报模型奠定了重要基础.     

传导网络中的地磁灾害（一）

地磁扰动可以破坏传导网络的运行，如电力系统、管线和通讯电缆。在电力系统中，地磁感应电流(GIC)通过电力变压器传到地面，干扰变压器的运行，使变压器变热，增加无功功率需求，并产生导致继电器误操作的谐波。在极端情况下，这些效应能导致电力中断，如1989年3月地磁暴期间，魁北克电网中断供电长达9个小时，600万人受到影响。地磁扰动是由太阳喷发高能粒子流向地球空间传动的结果。当这些粒子到达地球时，与地球磁场产生相互作用，所激发的电流向下流动到地球电离层。大部分强电流伴随着极光出现在横跨加拿大的东西带上。它是由电离层电流产生的磁场在地面上所看到的一种磁扰现象。预防地磁对电力系统的影响主要是阻止电力系统中产生地磁感应电流。但是这种措施相当昂贵，许多设施欲在地磁扰动期运行还需依赖地磁活动预报。加拿大地磁预报服务局是由加拿大自然资源部设立的机构，从1974年开始运行，现在可以提供覆盖加拿大3个纬度带的长期和短期地磁预报服务。该项研究工作是全方位的，从用于改进预报的有关太阳爆发的新资料到了解电力系统对磁扰的反应。地磁扰动研究由加拿大地磁预报中心和许多加拿大大学研究小组负责进行，而地磁感应的研究是由一些受其影响的行业组织进行的，也经常与上述预报中心进行合作研究。     

行星际扰动对地磁活动的影响

利用第23太阳活动周中WIND和ACE资料,统计分析行星际扰动对不同水平地磁活动的影响,研究磁暴强度与不同行星际参数之间的相关性,结果发现:①从长期来看,地磁活动指数Dst与太阳风速度的相关性最好,相关性在太阳活动谷年时最高;②多磁暴时序叠加结果证实了导致小、中、强磁暴开始的经验行星际南向磁场条件,磁暴过程中行星际磁场...     

2003年10～11月的大磁暴

分析了引起2003年10～11月发生的3个特大磁暴的太阳活动、行星际扰动以及中国东部地磁台链记录到的地面磁场变化。结果表明,这3个特别大的磁暴是由太阳质量抛射事件引起的。太阳向着地球喷发出的大量等离子体引起的强烈太阳风扰动和持续长时间的南向行星际磁场与磁层相互作用形成了特别大的磁暴。ACE卫星、GOES卫星以及地面地磁台站较完整地记录了这3次日地扰动传输过程。对于每一个磁暴,中国东部地磁台链记录到的H分量变化形态一致,纬度最高的满洲里地磁台H幅度最大,而其他台站的幅度与纬度无明显关系,这表明磁暴的发展不完全由赤道环电流引起,在这样强烈的磁暴期间,磁层内的电流体系非常复杂。     

基于地磁台站数据对磁暴期间环电流和场向电流的分布特征研究

磁暴的发生与环电流的变化密切相关.除了对称环电流外,部分环电流在磁暴的发展过程中也起到了重要的作用,同时部分环电流通过场向电流与极区电离层中的电流形成回路.本文应用INTERMAGNET地磁台网北半球中低纬区域地磁台站数据,对不同强度4个磁暴事件主相和恢复相期间部分环电流和场向电流的磁地方时分布进行了分析和讨论.对于每一个磁暴事件,在低纬地区（地磁纬度约0°—40°N）选用地磁经度上大致均匀的8个台站,通过坐标转换计算平行于磁偶极轴的地磁场水平分量H来分析磁暴期间环电流所引起的磁场扰动;在低纬地区8个台站的基础上增加中纬地区（地磁纬度约40°N—60°N）地磁经度上大致均匀的6个台站,计算地磁坐标系下地磁场东西分量Y来分析磁暴期间场向电流在中低纬地区引起的磁场扰动.结果表明,磁暴主相期间的部分环电流主要作用于磁地方时昏侧和夜侧扇区,并且主相和恢复相期间部分环电流引起的磁场变化随着磁暴级别的增大而增大;磁暴主相期间向下的场向电流多出现在夜侧至晨侧扇区,向上的场向电流多出现在昏侧至午后扇区,且中纬地区向下和向上场向电流的展布范围明显大于低纬地区;恢复相期间弱、中磁暴事件的场向电流呈现与部分环电流相同的减弱趋势,而强、大磁暴事件在恢复相末期场向电流引起的磁场变化明显不同于恢复相的其他时刻,这可能与高纬较强的亚暴活动有关.     

利用地磁脉动预报地球同步轨道相对论电子通量的方法研究

本文利用低纬地磁台站的Pi1、Pi2地磁脉动（Pi1-2）资料和地球同步轨道的Pc5地磁脉动资料,对2004年1月到2006年12月38个磁暴事件的地磁脉动参数进行了统计分析.在此基础上,考虑相对论电子的局部加速机制,并加入损失机制,建立了一个初步的磁暴期间地球同步轨道相对论电子通量对数值的预报模型.利用该模型,我们对上述38个磁暴事件进行预报试验,最优化结果是：相对论电子通量对数值的预测值和观测值之间的线性相关系数为0.82,预报效率为0.67.这说明该模式具有较好的预报效果,也表明利用地磁脉动参数进行相对论电子通量预报是可行的.     

中国区域GPS单频点定位在不同类型磁暴主相期间定位性能分析

地磁暴期间,电离层可出现不同程度的扰动,显著影响GNSS导航系统性能.本文针对GNSS系统应用需求,全面分析了不同等级磁暴主相期间GPS单频点定位精度在中国区域(地磁中、低纬地区)的受扰情况.结果表明,定位误差极端值的出现概率与磁暴等级呈正相关,也与测站纬度相关(低纬一般高于高纬),定位精度在U(垂直)方向受影响程度明显强于其他方向,且在磁暴恢复相期间定位精度也可能受到显著影响.上述研究结果对了解磁暴期间中国区域(地磁中、低纬地区)GNSS应用性能、北斗三号全球系统在中国区域的应用性能及系统升级和中国区域电离层扰动特性研究有参考价值.     

第23太阳活动周期太阳风参数及地磁指数的统计分析

日冕物质抛射(Coronal Mass Ejection,简称CME)和共转相互作用区(Corotating Interaction Region,简称CIR)是造成日地空间行星际扰动和地磁扰动的两个主要原因,提供了地球磁暴的主要驱动力,进而显著影响地球空间环境.为深入研究太阳风活动及受其主导影响的地磁活动的时间分布特征,本文对大量太阳风参数及地磁活动指数的数据进行了详细分析.首先,采用由NASA OMNIWeb提供的太阳风参数及地磁活动指数的公开数据,通过自主编写matlab程序对第23太阳活动周期(1996-01-01—2008-12-31)的数据包括行星际磁场Bz分量、太阳风速度、太阳风质子密度、太阳风动压等重要太阳风参数及Dst指数、AE指数、Kp指数等主要的地磁指数进行统计分析,建立了包括269个CME事件和456个CIR事件列表的数据库.采用事例分析法和时间序列叠加法分别对两类太阳活动的四个重要太阳风参数(IMF Bz、太阳风速度、太阳风质子密度、太阳风动压)和三个主要地磁指数(Dst、AE、Kp)进行统计分析,并研究了其统计特征.其次,根据Dst指数最小值确定了第23太阳活动周期内的355个孤立地磁暴事件,并以Dst指数最小值为标准将这些磁暴进一步分类为145个弱磁暴、123个中等磁暴、70个强磁暴、12个剧烈磁暴和5个巨大磁暴.最后,采用时间序列叠加法对不同强度磁暴的太阳风参数和地磁指数进行统计分析.统计分析表明,对于CME事件,Nsw/Pdyn(Nsw表示太阳风质子密度,Pdyn表示太阳风动压)线性拟合斜率一般为正;对于CIR事件,Nsw/Pdyn线性拟合斜率一般为负,这可作为辨别CME和CIR事件的一种有效方法.从平均意义上讲,相较于CIR事件,CME事件有更大的南向IMF Bz分量、太阳风动压Pdyn、AE指数、Kp指数以及更小的Dstmin.一般情况下,CME事件有更大的可能性驱动极强地磁暴.总体而言,对于不同强度的地磁暴,Dst指数的变化呈现出一定的相似性,但随着地磁暴强度的增强,Dst指数衰减的速度变快.CME和CIR事件以及其各自驱动的地磁暴事件有着很多不同,因此,需要将CME事件驱动的磁暴及CIR事件驱动的磁暴分开研究.建立CME、CIR事件及地磁暴的数据库以及获取的统计分析结果,将为深入研究地球磁层等离子体片、辐射带及环电流对太阳活动的响应特征提供有利的帮助.     

北京台磁暴出现频次及△Z/△H的初步分析/

本文利用北京台1957-1978年共22年的磁暴资料,统计分析了磁暴出现频次及△Z/△H随世界时、季节和年份的变化,初步研究了它们的频谱和与太阳活动性的关系,获得了可供磁暴预报与地磁预报地震探索研究参考的若干有意义的结果。      

1991年3月24日磁暴期间南极地区地磁脉动的分析

重点分析了1991年3月24日在南极中山站和长城站观测到的丰富的地磁脉动现象,给出了各种地磁脉动发生的时间和主要特征,并对两站各种地磁脉动做了比较分析．这不仅可以认识磁暴期间南极地区向日面与背日面、高纬与中纬地磁脉动的不同表现,也帮助我们了解南极地区磁暴期间地磁脉动形态和磁暴过程的关系。     

Magnetic fields in the Galaxy

Abstract

Methods of measuring magnetic field strengths in astrophysics are reviewed. These determine that a magnetic field of 2–3μG lies approximately along the local spiral arm of the Galaxy. Faraday rotation measures indicate that abrupt field reversals occur in a number of directions. At the centre of the Galaxy, the field is vertical, i.e. perpendicular to the plane of the Galaxy.     

Magnetic Fluctuations for Small Magnetic Prandtl Numbers

Numerous studies of magnetic fluctuations with a zero mean-field for small magnetic Prandtl numbers (Pr _m 1) show that magnetic fluctuations cannot be generated by turbulent fluid flow with the Kolmogorov energy spectrum. In addition, the generation of magnetic fluctuations with a zero mean-field for Pr _m 1 were not observed in numerical simulations. However, in astrophysical plasmas the magnetic Prandtl numbers are small and magnetic fluctuations are observed. Thus a mechanism of generation of magnetic fluctuations for Pr _m 1 still remains poorly understood. On the other hand, in astrophysical applications (e.g., solar and stellar convection zones, galaxies, accretion disks) the turbulent velocity field cannot be considered as a divergence-free. The generation of magnetic fluctuations by turbulent flow of conducting fluid with a zero mean magnetic field for Pr _m 1 is studied by means of linear and nonlinear analysis. The turbulent fluid velocity field is assumed to be homogeneous and isotropic with a power law energy spectrum ( k ^–p ) and with a very short scale-dependent correlation time. It is found that magnetic fluctuations can be generated when the exponent p > 3/2. It is shown also that the growth rates of the higher moments of the magnetic field are larger than those of the lower moments, i.e., the spatial distribution of the magnetic field is intermittent. In addition, the effect of compressibility (i.e., u 0) of the low-Mach-number turbulent fluid flow u is studied. It is demonstrated that the threshold for the generation of magnetic fluctuations by turbulent fluid flow with u 0 is higher than that for incompressible fluid. This implies that the compressibility impairs the generation of magnetic fluctuations. Nonlinear effects result in saturation of growth of the magnetic fluctuations. Asymptotic properties of the steady state solution for the second moment of the magnetic field in the case of the Hall nonlinearity for the low-Mach-number compressible flow are studied.     

地球磁层的磁场模型

1958年卫星探测发现了磁层,至今已有半个世纪,对磁层电场、电流体系、磁场、粒子分布和等离子体波的探测研究构成了空间物理的重要内容,其结果是各种磁层模型的出现.本文简要综述磁层磁场建模的基本原理、方法和发展历史,对十几种重要的磁层模型的特点、局限性和适用范围进行了对比分析,以Tyganenko模型为例,讨论了磁层模型发展的趋势.     

Magnetic Anomalies on the Tree Trunks

Magnetic measurements of soil and tree bark adjacent to a busy highway revealed a significant variation in the concentration of magnetic particles with distance from the highway. Further more, forest-facing tree-bark contains significantly more magnetic particles than road-facing tree-bark. Magnetic particles were detected both on the bark of the maple trees and in the first centimeter of the soil cover (O/A horizon). Stability of saturation isothermal magnetization (SIRM) and hysteresis parameters of the soil indicates the presence of single domain (SD/PSD) magnetic carriers. Measurements of the tree bark hysteresis parameters and SIRM detect a significant lower coercivity component that we interpret to be an indication of more abundant pseudo-single domain (PSD) type magnetic grains. Magnetic measurements around the perimeters of eight tree trunks reveal magnetic carriers whose distribution is antipodal to the source direction (highway). We interpret our observation by adopting an air circulation model, where suspended PSD/SD particles are carried in the air stream. The air stream from the heavy traffic lowers the amount of moisture on the tree trunk surfaces facing the highway and thus reduces an adhesive potential on this side. Therefore, more particles can stay on the moist side of the trunk protected from the direct airflow.     

Magnetic perturbations before the strong earthquakes

The search for the magnetic precursors of earthquakes by the method of synchronous detection is described. The data of the Guam Observatory (13.6°N, 144.9°E) located in a seismically active region and the USGS/NEIC catalogue of the National Earthquake Information Center of the U.S. Geological Survey for the period from 1991 to 2009 are used. Earthquakes with magnitudes M ≥ 7 in the range of longitudes from 100° to 170°E are analyzed. The intervals of accumulation cover 40 hours before and 40 hours after an earthquake. The preliminary result reveals an enhancement of fluctuations in the Z-component within 12 hours before the earthquake.     

Magnetic buoyancy and the Boussinesq approximation

Abstract

The full Boussinesq equations for hydromagnetic convection are derived and shown to include the effects of magnetic buoyancy. Instabilities caused by magnetic buoyancy are analyzed and their roles in double convection are brought out.     

Magnetic coupling in the solar system

Sarah Matthews, Danielle Bewsher and Chris Davis discuss the complexities of the solar magnetic field, informed by data from Hinode and STEREO.     

Effect of Stress on the Magnetic Memory of Induced Magnetic Anisotropy of Rocks and Its Mathematical Model

When re-heated to temperatures below the Curie temperature and subsequently cooled in a constant magnetic field (H _T), rock samples which contain magnetic minerals can acquire an induced magnetic anisotropy (IMA). As the result of acquiring the IMA, a constriction develops in the hysteresis loop of the magnetization of these rocks at the values of the magnetizing field close or equal to the HT. Thus the IMA is capable of retaining the information on the palaeointensity of the geomagnetic field, i.e., if IMA was created in a rock in the geomagnetic field in a past geological epoch, it preserves the information on the intensity of that field. Investigations have shown, that when IMA is created in a rock under external stress, the stress has an impact on the magnetic memory. Here we also deal with the issue of how stress affects the magnetic memory of IMA. A mathematical model for the effect of stress on magnetic memory phenomena related to induced magnetic anisotropy in rocks containing multidomain magnetite and titanomagnetite grains is proposed herewith. The effect of temperature on the magnetic memory of rocks is discussed also.     

Variations in the Intensity of the Earth's Magnetic Field

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.     

Magnetic storms

This talk provides a brief summary of the first conference devoted entirely to magnetic storms. The conference was held in Pasadena, California, at the Jet Propulsion Laboratory, 12-16 February 1996. Topics covered the relevant time-varying phenomena at the sun/corona, propagation of these structures through interplanetary space, the response of the magnetosphere from its interaction with these interplanetary structures, the formation of the storm- time ring-current (in particular the oxygen content of the ring-current), and storm ionospheric effects and ground based effects. A complementary summary is provided by Gonzalez et al. in EOS, 1996. The full set of review articles will be published in an AGU monograph and many of the contributed articles will appear in a special section of the Journal of Geophysical Research, Space Physics.