磁暴期间几种主要磁扰成分的演化特征

本文利用中国地磁子午链台站的资料,对1997～1999年期间发生的25次磁暴,用自然正交分量法（NOC）、相关分析和傅里叶分析三种方法,分3个步骤依次分离出依赖于世界时（UT）的暴时变化（Dst）、依赖于地方时（LT）的太阳静日变化（Sq）和太阳扰日变化（SD）.对各种变化时空特征的分析表明：①Dst变化清楚地反映出赤道对称环电流磁扰的空间分布和时间演化特征;②满洲里、北京十三陵和琼中台Sq幅度在多数磁暴主相期间出现极大和极小值,反映了Sq焦点在纬度方向上的移动所产生的地磁效应;③SD变化在主相期间最强,在恢复相期间逐渐减弱;④相关分析和傅里叶分析提供了一种能有效提取Sq和SD变化的方法.     

中国地磁台观测的2014年地磁急变

地磁急变（jerk）是起源于地球外核并在导电地幔过滤效应后在地球表面观测到的一种地磁现象,其反映了地核内部某些动力学过程.Jerks在空间范围上既可以是区域性的,也可以是全球性的.中国地区地磁台能否检测到2014年jerk？针对这一问题,利用中国大陆10个地磁台的磁静日月均值和CHAOS-6全球磁场模型,分析了X、Y和Z分量2008—2018年期间的长期变化,估算了2014年前、后的长期加速度值,确定了2014年地磁jerk的时间和强度.研究表明中国地磁台Y分量的长期变化为"Λ"型,Z分量存在明显的"V"型,具有典型的jerk特点.Y分量jerk出现的时间大约在2014年6月,比非洲大陆的Algeria TAM台和南美洲French Guiana KOU台时间滞后大约4个月.这暗示着产生jerks的地核流体波动的时序特点.中国西部和东北部地磁台的长期变化形态有明显的差别,主要由非偶极磁场引起.CHAOS-6模型与地面台站的长期变化形态并非始终一致.本文结果有助于更好地理解和解释长期变化的时间演变和地理分布,并为深入探讨jerks的地核起源和驱动机制提供新的观测约束.     

中国地磁台观测的2014年地磁急变

地磁急变（jerk）是起源于地球外核并在导电地幔过滤效应后在地球表面观测到的一种地磁现象,其反映了地核内部某些动力学过程.Jerks在空间范围上既可以是区域性的,也可以是全球性的.中国地区地磁台能否检测到2014年jerk？针对这一问题,利用中国大陆10个地磁台的磁静日月均值和CHAOS-6全球磁场模型,分析了X、Y和Z分量2008—2018年期间的长期变化,估算了2014年前、后的长期加速度值,确定了2014年地磁jerk的时间和强度.研究表明中国地磁台Y分量的长期变化为"Λ"型,Z分量存在明显的"V"型,具有典型的jerk特点.Y分量jerk出现的时间大约在2014年6月,比非洲大陆的Algeria TAM台和南美洲French Guiana KOU台时间滞后大约4个月.这暗示着产生jerks的地核流体波动的时序特点.中国西部和东北部地磁台的长期变化形态有明显的差别,主要由非偶极磁场引起.CHAOS-6模型与地面台站的长期变化形态并非始终一致.本文结果有助于更好地理解和解释长期变化的时间演变和地理分布,并为深入探讨jerks的地核起源和驱动机制提供新的观测约束.     

The solar causes of the occurrence of selected geomagnetic storms and geomagnetic quiet

Резюме Приводится общее толкование возникновения геомагнитного покоя и геомагнитнЫх бурь на основании новЫх гипотез, разработаннЫх в Геофизическом институте ЧСАН. Приводятся некоторые случаи геомагнитного покоя. Что касается примеров геомагнитнЫх бурь, то здесь имеются в виду прежде всего такие бури, которЫе в литературе обозначаются как “проблема” бурь, далее бури для которЫх существует несколько иногда даже противоречивых толкований По рассматриваемому здесь способу можно бЫло бЫ истолковать любую геомагнитную бурю, равно как и небольшое возмущение. Для этого необходимоо располагать точным даннЫми относительно солнечной ситуации на ЦМ.

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Address: Boční II, Praha 4-Spořilov.     

The theory of geomagnetic induction

The theoretical basis of electromagnetic induction methods in geophysics is considered with special reference to the interplay of physical ideas and mathematical arguments. The design of mathematical problems to elucidate observed physical phenomena, and methods of solving them, are discussed. Earth models suitable for various types of investigation are considered. The importance of getting the correct physical interpretation of the solution of a mathematical problem is stressed.     

长春地磁台地磁场长期变化基本特征

长春地磁台从1957年开始进行正规地磁观测至今,地磁场的长期变化已完成了一个完整的下降、转折、上升的变化周期,这种长期变化是偶极场与非偶极场变化的叠加,以非偶极场变化为主体,并受东亚大陆磁异常场源强度及方向变化的控制和影响。     

The dynamics and thermodynamics of precipitation loading

A one-dimensional, time-dependent numerical cloud model is used to analyze the factors in the dynamic and thermodynamic equations which lead to a steady-state or nonsteady-state solution for the cloud vertical motion, buoyancy, precipitation, and cloud water fields. ‘Bulk water’ microphysical techniques are used for the cloud, rain, and hail variables. An atmospheric sounding from a severe storm situation is used as initial and environmental conditions, yielding model updrafts of 40 m sec^?1 maximum and more than 10 m sec^?1 over the entire cloud region. ‘Early conversion’ of the cloud water to rain leads to loading of lower portions of the updraft by rain, the formation of appreciable amounts of hail by freezing of the supercooled rain, and subsequent loading of the middle and upper portions of the updraft so that the updraft erodes throughout the cloud depth and the cloud dissipates, yielding a vigorous rain shower. A delay in the conversion of the cloud water to rain results in a steady-state solution, no rain or hail falling through the updraft. A two-dimensional cloud simulation of this same case shows rain and hail in the upper cloud regions recycled in the two-dimensional flow into the updraft near cloud base and a breakdown of the updraft with resultant rainout (negligible hail reaching the ground). The breakdown of the updraft has profound effects on the temperature field within the cloud, causing the lapse rate to deviate from the steady-state condition and approach the initial environmental conditions. The results emphasize the fact that the local change in temperature (and other dependent variables as well) is not independent of the vertical velocity, in general. This has implications for the interpretation of measurements made within clouds.     

第10代国际地磁参考场

国际地磁与超高层大气物理学协会（IAGA）于2004年12月12日发表了第10代国际地磁参考场（IGRF）。这是对地球主磁场标准数学描述的最新版本，在对地球深部、地壳、电离层及磁层的研究中有广泛应用。国际地磁参考场系数由国际地磁与超高层大气物理学协会的一个特别工作组最终确定下来。国际地磁参考场是地磁场模型工作者和全世界从事卫星及台站地磁观测数据收集和发布的单位共同努力的结果。     

太原基准地震台地磁背景噪声分析

太原基准地震台数字化地磁观测项目建成运行后,背景噪声水平较大,影响观测资料的使用.采取多种技术措施,认为地电阻率观测对地供电是地磁稳频干扰的主要成分,是地磁背景噪声的一项重要干扰因素.     

The fifth order geomagnetic multipole: The duotrigintupole

Summary The notion of a dipole is generalized to the case of the fifth order spherical harmonic coefficients of the geomagnetic potential. The corresponding five axes and fifth order multipole strength are computed for ten epochs in the interval 1845 to 1965.     

The fourth order geomagnetic multipole: The sedecimupole

Summary The nine coefficients of fourth order spherical harmonic functions in the expression for the potential of the main geomagnetic field are used to derive the nine parameters of a fourth order multipole. These nine parameters consist of the strength of the multipole, and four unit vectors or axes. The points of intersection of the axes with the surface of the Earth are called poles. Although movements of the poles over the period 1829 to 1965 are masked by random errors in the spherical harmonic coefficients, all of the axes show eastward components of drift since 1829, but two have drifted westward in later years to return almost to their initial 1829 positions. The strength of the fourth order multipole has shown a general increase, amounting to some 30 per cent of the 1829 value.     

The dynamics and thermodynamics of large ash flows

 Ash flow deposits, containing up to 1000 km³ of material, have been produced by some of the largest volcanic eruptions known. Ash flows propagate several tens of kilometres from their source vents, produce extensive blankets of ash and are able to surmount topographic barriers hundreds of metres high. We present and test a new model of the motion of such flows as they propagate over a near horizontal surface from a collapsing fountain above a volcanic vent. The model predicts that for a given eruption rate, either a slow (10–100 m/s) and deep (1000–3000 m) subcritical flow or a fast (100–200 m/s) and shallow (500–1000 m) supercritical flow may develop. Subcritical ash flows propagate with a nearly constant volume flux, whereas supercritical flows entrain air and become progressively more voluminous. The run-out distance of such ash flows is controlled largely by the mass of air mixed into the collapsing fountain, the degree of fragmentation and the associated rate of loss of material into an underlying concentrated depositional system, and the mass eruption rate. However, in supercritical flows, the continued entrainment of air exerts a further important control on the flow evolution. Model predictions show that the run-out distance decreases with the mass of air entrained into the flow. Also, the mass of ash which may ascend from the flow into a buoyant coignimbrite cloud increases as more air is entrained into the flow. As a result, supercritical ash flows typically have shorter runout distances and more ash is elutriated into the associated coignimbrite eruption columns. We also show that one-dimensional, channellized ash flows typically propagate further than their radially spreading counterparts. As a Plinian eruption proceeds, the erupted mass flux often increases, leading to column collapse and the formation of pumiceous ash flows. Near the critical conditions for eruption column collapse, the flows are shed from high fountains which entrain large quantities of air per unit mass. Our model suggests that this will lead to relatively short ash flows with much of the erupted material being elutriated into the coignimbrite column. However, if the mass flux subseqently increases, then less air per unit mass is entrained into the collapsing fountain, and progressively larger flows, which propagate further from the vent, will develop. Our model is consistent with observations of a number of pyroclastic flow deposits, including the 1912 eruption of Katmai and the 1991 eruption of Pinatubo. The model suggests that many extensive flow sheets were emplaced from eruptions with mass fluxes of 10⁹–10¹⁰ kg/s over periods of 10³–10⁵ s, and that some indicators of flow "mobility" may need to be reinterpreted. Furthermore, in accordance with observations, the model predicts that the coignimbrite eruption columns produced from such ash flows rose between 20 and 40 km. Received: 25 August 1995 / Accepted: 3 April 1996     

The fluid dynamics and thermodynamics of eruption columns

A new model for Plinian eruption columns is derived from first principles and investigated numerically. The dynamics particular to the momentum-driven basal gas-thrust region and the upper buoyancy-driven convective region are treated separately. The thermal interactions in the column are modelled by the steady-flow-energy equation. The main results of the present paper are that: (1) the basal gas-thrust region model predicts a very rapid initial expansion of the material on leaving the vent; (2) the gas-thrust region height decreases with initial temperature, inital gas content of the erupted material and initial velocity, but increases with vent radius; (3) the total column height increases with initial temperature, initial velocity and vent radius, but decreases with initial gas content; (4) column collapse occurs for initial velocities of the order of 100 m/s; the precise value increases as the initial gas content in the erupted material decreases; (5) for large vent radii or low initial gas content of the erupted material, the velocity in the column can increase with height once in the buoyancy-driven region instead of decaying to zero monotonically; (6) the interaction of the potential energy with the enthalpy is found to be the dominant thermal interaction in the upper part of the column. Previous models of eruption columns involve inconsistencies and simplifications; these are shown to lead to significant differences in the results in comparison to the present model.     

Variation of lunar and solar geomagnetic tides with sunspot and geomagnetic activity

Summary Solar and lunar geomagnetic tides inH at Alibag have been determined by spectral analysis of discrete Fourier transforms following the method of Black and the well-known Chapman-Miller method. The seasonal variation inL ₂(H) is opposite to that inL ₂(D) with maximum in thed season and minimum in thej season. In bothH andD the enhancement due to sunspot activity is larger in lunar tide than in solar tide. Surprisingly, the enhancement due to magnetic activity is greater inL ₂(H) than inS ₁(H), while the contrary is true for declination. It is inferred that there is a local time component of the storm time variation contrary to the view expressed by Green and Malin. The enhancements in amplitudesL ₂ andS ₁ inH andD, due to sunspot activity and due to magnetic activity, have been separated. The results show that the amplitude at zero sunspot number increases with magnetic activity in all the four parameters, while the enhancement due to sunspot activity at different levels of magnetic activity decreases with increase ofK _p. But if bothK _p andR are increasing, whenK _p increases enhancement due toR decreases and whenR increases enhancement due toK _p decreases.     

地磁野外观测记录和回放软件的再研究

1　软件介绍本文软件的再研究设计和技术指标的编写是以《地震地磁野外测量规范》 (以下简称《规范》)为依据 ,并从地磁野外工作的特点和实用性出发。按要求地磁野外观测“组与组之间的时间间隔应不小于 5分钟”。为便于地磁数据的日变量图等进行通化处理 ,特规定每组地磁野外观测在一定的时间进行 (每时的 0 5分、 1 0分、 1 5分…… )。为达到这样的地磁野外观测的时间模式 ,地磁野外观测员或记录员就要准备能显示时、分、秒且走时较准确的电子表或其他电子时钟等。另外 ,时钟的时间和 PC-1 50 0 A的时钟要对准。PC-1 50 0 A所具有的ti…     

地磁场长期变化特征及机理分析

将地磁场的总变化分为三部分：偶极场自身变化,非偶极场自身变化及非偶极场磁斑区通过对核幔边界（CMB）层环形电流的调制来影响偶极场的变化. 本文利用国际地磁参考场模型IGRF）1900～2000计算分析了地球不同深度地磁场分布及长期变化特征,且讨论了变化的可能机制. 可以推论,地磁场西漂和倒转不仅是非偶极场引起,同时与偶极场有密切关系.