实测数据与标准地磁模型的比较

利用国际标准地磁模型,可以计算出任意点的磁场强度。本文对“风云一号”卫星的磁强计测量数据与标准地磁模型计算结果进行了平静期吻合性的比较。分析了地磁强度绝对值的地理分布规律以及平静期南大西洋磁异常区的数据变化情况,为进一步分析地磁扰动时期的变化情况打下基础。     

地磁定位方法综述

地磁导航具有可用区域广泛、无累积误差、无源和隐蔽性强等优势,是未来定位导航与授时(PNT)体系中潜在的重要导航定位手段之一。地磁导航技术包括磁场信息的测量、地磁基准图的建立和地磁定位方法的设计3个重要内容。本文主要围绕地磁定位方法,调研总结了当前主流的地磁滤波、地磁匹配和磁场同时定位与构图(SLAM)三类方法的原理及技术发展路线,重点分析了不同方法的优缺点、适用场景、时效性、对磁图和传感器的需求,并对地磁定位方法的发展方向进行了展望。     

基于多参量信息的水下地磁滤波导航算法

由于水下运载器使用地磁滤波导航方法时难收敛、易发散,根据水下运载 器的特点设计了一种基于多参量信息的水下地磁滤波导航算法。针对单纯使用地磁数据 进行位置匹配精度较差的问题,该算法在匹配及滤波过程中引入了地磁强度、航向、航 速等多参量信息,采用非线性滤波框架进行信息融合,采用粒子群算法根据多参量信息 进行位置搜索,并以之为系统滤波的观测值,通过提高位置观测精度改进滤波的收敛性 和鲁棒性。仿真结果表明,算法滤波精度高,稳定性好,能够较好地抑制各类传感器干 扰和误差对滤波估计的影响,适用于水下运载器的地磁导航定位。     

地磁定位方法综述

地磁导航具有可用区域广泛、无累积误差、无源和隐蔽性强等优势,是未来定位导航与授时（PNT）体系中潜在的重要导航定位手段之一。地磁导航技术包括磁场信息的测量、地磁基准图的建立和地磁定位方法的设计3个重要内容。本文主要围绕地磁定位方法,调研总结了当前主流的地磁滤波、地磁匹配和磁场同时定位与构图(SLAM)三类方法的原理及技术发展路线,重点分析了不同方法的优缺点、适用场景、时效性、对磁图和传感器的需求,并对地磁定位方法的发展方向进行了展望。     

基于概率数据关联的地磁匹配算法

针对轮廓匹配算法存在的虚定位问题,在轮廓匹配算法的基础上,提出了一个新的分批地磁匹配方法——基于概率数据关联滤波的地磁匹配算法。算法把满足一定条件的相关值作为滤波器的有效量测,把巡航导弹的位置作为状态变量,建立了基于概率数据关联的地磁匹配模型,利用概率数据关联滤波算法计算巡航导弹的位置坐标。仿真结果表明,该算法有效地降低了虚定位发生的概率,正确匹配率、导航效果均优于轮廓匹配算法。     

地磁测量数据野值的辨识与剔除

针对地磁测量野值的辨识与剔除方法进行了深入研究。分析了野值辨识与剔除的基本原理,基于孤立型野值和斑点型野值模型分析比较了不同的野值剔除方法。利用地磁场实测信息,优化了野值剔除方法的参数,并从不同角度验证了方法的野值修复效果。仿真结果表明,在观测信息为总强度地磁信息条件下,优化的最小二乘B样条逼近法能够有效地辨识野值,具有较好的野值修复效果。     

飞行器组网多维地磁匹配的相关度算法

地磁匹配导航技术是跨海飞行器的自主导航方式之一。海洋磁场强度平滑、区域变化较大的特点,使得飞行器一维地磁匹配方法难以应用于飞行器自主导航。在跨海飞行器组网条件下,讨论了多维地磁匹配相关度算法,并仿真计算了多维地磁匹配相关度的匹配时间、匹配概率,计算表明多维地磁匹配相关度算法优于单航迹匹配相关度;在相同概率下区域内370 m×370 m网格匹配时间短、匹配概率高。飞行器组网多维地磁匹配的相关度算法研究为海洋区域地磁匹配导航应用提供参考。     

基于网络中心的航空地磁观测的几个技术问题

地磁场是深入研究最多的地球物理场之一,携带着诸多地球物理学信息,目前地磁观测在防震减灾、资源勘探、地磁导航、水下目标探测等领域有着广泛应用。与卫星磁测相比,飞机、浮空器等航空平台具有航路可规划、观测高度低、受外太空磁干扰小等优点。但是,发展网络环境下的空基地磁观测,遇到了新的技术问题,本文从航电综合的角度,给出了解决这些技术难点的可行途径。     

一种导弹捷联惯导/地磁/雷达高度表组合导航方法

基于雷达高度表和磁强计的测量信息,提出一种弹道导弹捷联惯导/地磁/雷达高度表组合导航方法。以磁强计测量值与磁场模型的磁场强度值之差和高度表与惯导解算高度之差作为量测,只用一个观测表达式即可同时包含载体的姿态及位置信息。引入状态反馈,利用混合校正的Kalman滤波得到系统导航信息的最优估计。仿真结果表明,该算法能有效抑制捷联解算误差的发散,当磁强计精度为100nT,雷达高度表精度为50m时,仿真1000s后姿态精度优于20′,定位精度为2.68 km。该导航方法自主性高,精度较高,具有一定工程应用价值。     

世界地磁模型在飞行管理系统中的应用

飞行管理系统采用真北基准作为方位角的参考基准,针对飞行员可选择方位角的输入或输出基准为磁北基准的问题,采用引入世界地磁模型计算空间某地理点的磁差的方法,将方位角在真北和磁北基准之间进行转换,并分析了飞行高度对磁差计算精度的影响。结果表明:采用世界地磁模型计算的磁差精度满足MIL-W-89500规范要求,世界地磁模型可以应用于飞行管理系统中。     

Geomagnetic pulsations

Conclusion In writing this review paper the author has been aware that although the present international classification on geomagnetic pulsations (see Table I) had been really useful for several years since the Berkeley Meeting, it seems unsuitable for the up-to-date pulsation study. This is mainly due to the fact that it depends only on the period and waveform of the pulsations. For example, (1) occurrence of PP type of Pc1 even in the international Pc3 range (Heacock, 1966), (2) PP and CE getting mixed in a common period band (cf. 2.7), (3) similar mixing tendency of Pc3 with Pc4 (cf. 3.3 or Figure 21), (4) subtypes of Pi pulsations having common period ranges but different source mechanisms, (5) existence of various types of pulsations which can be classified neither to Pc nor to Pi (cf. Section 6), and so on. Hence the author feels that a new pulsation classification based on physical image on the occurrence models is really needed now.According to the international definition which has a period range of pulsations from 0.2 (5 Hz) to 600 sec, a part of the following electromagnetic field fluctuations called ELF emissions and ELF whistlers should belong to geomagnetic pulsations. ELF emissions are at times observed near 4 Hz and 9 Hz. They are so termed because of the difference between these frequencies and the Schumann resonance frequencies of 8 and 14 Hz (Yanagihara and Shimizu, 1969; Polk, 1969). Another type, ELF whistlers, exhibit either rising, falling or fluctuating tones from about 2 Hz to probably a few tens of Hz (Duffus, Nasmyth et al., 1958; Yamashita, 1967; Glangeaud, 1967; Yanagihara and Shimizu, 1969). In this review paper, however, both ELF emissions and whistlers have not been reviewed, since most of these seem to be out of the international frequency range so far as present observational knowledge is concerned. Some of the Pc6 and Dp2, involved in the international period range of pulsations, have also not been commented on, but the reader is advised to refer to Herron (1967) and Nishida (1968), respectively, for more detail.It has been frequently pointed out in this paper that latitudinal dependence of pulsation amplitude is one of the most important clues for seeking the model of excitation and propagation of HM and EM waves, but that this dependence has not been precisely obtained so far owing to the difference in geomagnetic longitude of the pulsation stations (for example, see Figure 40). Cooperative observations based on standardized magnetometers are eagerly desired at stations which are densely arranged along the same magnetic meridian, even if the observation is temporal.As already reviewed, various conflicting models have been proposed for each type of pulsation. On the occurrence of pc's, for example, there are two main conflicting models. In the first model, Pc2, 3, and 4 (Troitskaya, 1967; Patel and Hastings, 1968; and others) or Pc3 and 4 (Radoski and Carovillano, 1966) are related to one and the same resonance system and the difference in the type of these pc's is attributed to an effect of geomagnetic activity on the size of this system. In the second model, Pc2, 3, 4 and 5 are related to three or four different resonant systems (Jacobs and Sinno, 1960b; Hirasawa and Nagata, 1966; Kato, Mori et al., 1968; and others). Most of the conflict among such models seems to be removable by combining more thorough theoretical studies and correct dynamic spectrum analyses of the data at the polar region, auroral zone, sub-auroral zone, and middle and low latitudes, for various geomagnetic disturbance conditions.     

地磁导航技术研究进展

地磁场是地球的固有资源,利用地磁场匹配进行导航是一种新型导航技术.与传统的惯性导航和卫星导航比较,地磁导航具有无积累误差、抗干扰、隐蔽性好、导航信息丰富等优势.文章介绍了地磁导航的3个基本要素,即磁场测量技术、地磁模型以及定位与导航技术.分析了弱磁场磁力仪在地磁导航中的应用及其优缺点,讨论了地磁场模型和地磁匹配算法,展望了地磁导航技术的应用前景.     

Geomagnetic Core Field Secular Variation Models

We analyse models describing time changes of the Earth’s core magnetic field (secular variation) covering the historical period (several centuries) and the more recent satellite era (previous decade), and we illustrate how both the information contained in the data and the a priori information (regularisation) affect the result of the ill-posed geomagnetic inverse problem. We show how data quality, frequency and selection procedures govern part of the temporal changes in the secular variation norms and spectra, which are sometimes difficult to dissociate from true changes of the core state. We highlight the difficulty of resolving the time variability of the high degree secular variation coefficients (i.e. the secular acceleration), arising for instance from the challenge to properly separate sources of internal and of external origin. In addition, the regularisation process may also result in artificial changes in the model norms and spectra. Model users should keep in mind that such features can be mis-interpreted as the signature of physical mechanisms (e.g. diffusion). Finally, we present perspectives concerning core field modelling: imposing dynamical constraints (e.g. by means of data assimilation) reduces the non-uniqueness of the geomagnetic inverse problem.     

Geomagnetic Tracing of the Inner Heliosphere

Historical data of the geomagnetic activity records in St. Petersburg since 1841 do not show any ‘doubling’ of the total magnetic field at the Sun as claimed recently by Lockwood et al. (1999). However, recurrent patterns of the geomagnetic activity variations display ‘secular’ trend of the solar wind near ecliptic plane resulting from gradual change of the topological structure of the solar corona (Ponyavin, 1997). By comparing geomagnetic and eclipse observations we found ‘typical’ coronal shapes, which correspond better to periods of extremely low and high geomagnetic activity level rather than standard sunspot activity referencing as ‘Corona at Solar Maximum or Minimum’. Using geomagnetic records as proxies it has been suggested that the maximum of the sunspot activity was in July 2000. This revised version was published online in August 2006 with corrections to the Cover Date.     

Geomagnetic induction effects in ground-based systems

Plasma physics processes, whose ultimate origin is the Sun, exist in the Earth's magnetosphere and ionosphere and can produce effects which are detrimental to the operation of technological systems associated with long conductors deployed on the Earth's surface. Geomagnetic fluctuations produced by such plasma processes can cause disturbances and disruptions in cable communication systems, electrical power distribution systems, and long pipelines. This paper briefly addresses these three topics with illustrative examples of some measured effects from each topic area.