Solar magnetic activity: topology and prediction

We ascribe the solar magnetic activity to the interplay between the plasma flow and the magnetic field. Observations by SOHO, Hinode and upcoming SDO are discussed. We then discuss the understanding and modeling of solar magnetic activity based on mathematical topological concepts. We present predictions using neural networks. Further we describe the outcome of the cycle 24 prediction panel. Finally, recommendations are given for making improved predictions.     

The correlation between geomagnetic disturbances and topology of quasi-open structures in the solar magnetic field

Results of photospheric magnetic field extrapolation in a potential approximation and of the technique for separating the open part of magnetic flux have revealed that changes in the relationship between the open part of the south polarity magnetic flux obtained in the chromosphere and corona from July to November 2006 correlate with variations in the Akasofu parameter calculated from data on the solar wind parameters and interplanetary magnetic field at Lagrange point L1, and with the K _p index.     

Complexity,magnetic field topology,criticality, and metastability in magnetotail dynamics

Recently, it has been shown that certain features of magnetotail dynamics in response to solar wind changes may resemble the behavior of a complex system near a dynamical critical state (Chang, Phys. Plasmas 6 (1999) 4137; Consolini and Chang, Space Sci. Rev. 95 (2001) 309), and of topological phase transitions (Chang, Phys. Scr. (2001), 80). Moreover, the impulsive part of the magnetotail response seems to be well described by cellular automata and other simulation models displaying criticality.Here, the relevance of the magnetic field topological disorder will be discussed in connection with observed complexity and near-criticality, showing how the impulsive character of the magnetotail response could be viewed as fluctuation-induced topological transitions among metastable configurations of magnetic field topology.     

Probing the magnetic topology of coronal mass ejections by means of Ulysses/HI-SCALE energetic particle observations

In this work, solar flare energetic particle fluxes (E_e 42 keV) observed by the HI-SCALE instrument onboard Ulysses, a spacecraft that is probing the heliosphere in 3-D, are utilized as diagnostics of the large-scale structure and topology of the interplanetary magnetic field (IMF) embedded within two well-identified interplanetary coronal mass ejection (ICME) structures. On the basis of the energetic solar flare particle observations firm conclusions are drawn on whether the detected ICMEs have been detached from the solar corona or are still magnetically anchored to it when they arrive at 2.5 AU. From the development of the angular distributions of the particle intensities, we have inferred that portions of the ICMEs studied consisted of both open and closed magnetic field lines. Both ICMEs present a filamentary structure comprising magnetic filaments with distinct electron anisotropy characteristics. Subsequently, we studied the evolution of the anisotropies of the energetic electrons along the magnetic field loop-like structure of one ICME and computed the characteristic decay time of the anisotropy which is a measure of the amount of scattering that the trapped electron population underwent after injection at the Sun.     

The primary magnetic remanence of a dolerite sill from northeast Spitsbergen

An Upper Jurassic dolerite sill from Lomfjord, northeast Spitsbergen, has been submitted to rock- and palaeomagnetic studies. In the cooling stage the original titanomagnetite underwent a high-temperature alteration forming exsolution of ilmenite lamellas. Due to rapid cooling the border zones in part escaped the high-temperature alteration but instead low-temperature oxidation, producing at least a low-temperature metastable magnetic mineral, is fairly pronounced in these parts of the sill. Thermal demagnetization has established that both mineral phases carry the same general magnetization direction suggesting the total remanence (reverse) to be of deuteric origin. Consideration of the cooling rate indicates that the accumulated geomagnetic secular variation may cover a time span of the order of 10³ years. The relative pole position is at 61°N, 210°E, a result which is in agreement with some other Mesozoic results from Spitsbergen, but in rather marked disagreement with other published data for the Mesozoic of Europe.     

地磁钩扰的全球响应特征研究与初步统计结果

地磁钩扰是太阳耀斑效应的直观表现之一, 其研究有助于深入理解太阳爆发对地球空间环境的影响过程, 并能为空间天气建模和预报提供科学依据.本文利用山东大学威海地磁台和Intermagnet地磁链与子午工程的地磁观测数据, 联合GOES卫星及数字测高仪等的数据, 研究了一个由M5.6级太阳耀斑引发的地磁钩扰事件的全球响应特征.研究发现:地磁钩扰特征呈现出南北半球与午前/午后的差异, 且地磁响应相对于太阳耀斑存在约3 min的滞后现象, 而夜侧无明显扰动; 利用位于日侧的50余个地磁台站的数据统计分析后发现地磁钩扰幅度呈现正态分布, 且在当地时正午附近达到峰值; 利用地磁数据反演出钩扰发生时电离层的电流体系S_s和宁静日电流S_q, 并用该电流体系解释了此事件中地磁数据的变化特征.另外, 本文初步统计了1996-2015年的地磁钩扰事件数以及相关的太阳耀斑事件数, 分析后发现X级耀斑引发地磁钩扰的可能性最大, 达42%, 由M级耀斑引发的地磁钩扰事件数最多, A、B、C级等小耀斑引发地磁钩扰的可能性很小.

     

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...     

The Martian magnetic field

The magnetic field measurements of the Mars 2, 3 and 5 spacecraft have been interpreted by Dolginov and co-workers to be consistent with an intrinsic planetary magnetic moment of 2.5 × 10²² gauss cm³. They base this interpretation mainly on the apparent size of the obstacle responsible for deflecting the solar wind, the lack of dependence of the sign of the magnetic field in the wake region of the planet on the sign of the component of the interplanetary field radially out from the sun, and an apparent encounter of the Mars spacecraft with the planetary field. When examined in detail this evidence is very suspect. A detailed criticism of the arguments by Dolginov and co-workers for an intrinsic field has appeared elsewhere. Herein we summarize this criticism and present, in an appendix, a compendium of the Mars 3 and 5 magnetic field data transformed into a coordinate system in which the details of the interaction are more easily visualized. Many of these data have not been published in this form previously.     

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".     

The stability of dissipative magnetohydrodynamic shear flow in a parallel magnetic field

Abstract

Strong decay bounds are obtained for linearized perturbations to an unbounded, plane Couette flow in a parallel magnetic field. Finite conductivity and molecular viscosity are found to be stabilizing. Those modes decaying most slowly have the form of rolls aligned with the shear flow. The non-aligned rolls decay at an enhanced rate. Stability bounds at finite amplitude are obtained for flows bounded in one direction using energy methods.     

导电导磁层状介质上的固定翼航空瞬变电磁响应

基于电磁理论,导出了含介电参数、电导率参数和磁导率参数的导电导磁层状大地条件下的固定翼航空瞬变电磁响应的计算公式.编制了计算机程序,并对理论模型进行正演计算,根据计算结果分析了模型的介电常数、电阻率和磁导率参数、飞行高度参数对响应的影响.理论模型的计算结果显示当其它条件相同时,介质电阻率越小或磁导率越大,则航空电磁响应...     

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 emergence of braided magnetic fields

We study the emergence of braided magnetic fields from the top of the solar interior through to the corona. It is widely believed that emerging regions smaller than active regions are formed in the upper convection zone near the photosphere. Here, bundles of braided, rather than twisted, magnetic field can be formed, which then rise upward to emerge into the atmosphere. To test this theory, we investigate the behaviour of braided magnetic fields as they emerge into the solar atmosphere. We compare and contrast our models to previous studies of twisted flux tube emergence and discuss results that can be tested observationally. Although this is just an initial study, our results suggest that the underlying magnetic field structure of small emerging regions need not be twisted and that braided field, formed in the convection zone, could suffice.     

The sub-surface magnetic fields produced by a line current source on a non-flat earth

Summary A simple cylindrical model is employed to estimate the effect of non-flatness of the ground on the sub-surface electromagnetic field from a current-carrying cable on the surface. It is shown that, if the surface curvature is sufficiently small, the fields in the cylinder model are very similar to those for the conducting half-space model of the earth employed earlier. The results can be used to provide estimates of expected errors in electromagnetic direction-finding of a buried receiving terminal.The research reported here was supported in part by the Mine Safety Center, U.S. Bureau of Mines.     

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.     

Low-field variation of magnetic susceptibility as a tool for magnetic mineralogy of rocks

Low-field variation of magnetic susceptibility was investigated on a collection of several hundreds specimens of various minerals and rocks using the KLY-4S Kappabridge. The measurement is fully automated, being executed in 21 distinct fields ranging from 2 to 450 A/m (in one frequency of 875 Hz). The measurement is rapid, 7 min per specimen, so that large collections of specimens can be investigated. The results can be processed both graphically and mathematically. For the latter processing, parameters of two kinds were introduced. One characterizes the susceptibility change with field, the other one characterizes the field in which the susceptibility no longer obeys the Rayleigh law and starts becoming more complex.The results were evaluated statistically. Remarkable differences were revealed between individual minerals and between some rock types. For example, the field variation of susceptibility of pyrrhotite is in general an order of magnitude larger than that of titanomagnetite. The susceptibility increase in pyrrhotite starts at the field an order of magnitude lower than that of titanomagnetite. Low-field variation of susceptibility then appears as an interesting phenomeon that helps in the identification of magnetic minerals and in some cases also in assessing the compositional variation of them.     

磁变仪标度值自动测定电路的改进

介绍了改进后的磁变仪标度值自动测定电路的主要特性、电路工作原理和使用注意事项,提供了电路原理图。