On the geo-electromagnetic aspects of tornado initiation

Summary The reasoning that joule heating in multiple-stroke lightning flashes associated with an active tornado constitutes the major energy source for itsdrive is questioned. An electrical discharge is proposed as a mechanism for the formation of the initial vortexsink, a high specific-energy source being supplied by Joule heating in a leader-stroke coronal discharge of several hundred amperes and milliseconds duration. Magnetic pinch effects are invoked as a means of preventing large lateral heat losses from the ionised column and a resulting degradation of the energy source. Applying the equation for magneto-hydrostatic balance, it is shown that magnetic pinch exerted on the column by the current-induced magnetic field alone is insufficient to achieve balance and thus prevent energy losses. Qualitative arguments are used to demonstrate that the pinch effect can be enhanced through the interaction with the external, geomagnetic field. Observational evidence is presented to support the hypothesis of geomagnetic control for tornado initiation on a global scale. It is seen in large differences of tornado frequency between regions on the surface of the Earth featured by comparable pre-requisite thunderstorm frequency but significant differences in geomagnetic intensity which qualitatively agree with the predicted effect.     

The self-similar,non-linear evolution of rotating magnetic flux ropes

We study, in the ideal MHD approximation, the non-linear evolution of cylindrical magnetic flux tubes differentially rotating about their symmetry axis. Our force balance consists of inertial terms, which include the centrifugal force, the gradient of the axial magnetic pressure, the magnetic pinch force and the gradient of the gas pressure. We employ the “separable” class of self-similar magnetic fields, defined recently. Taking the gas to be a polytrope, we reduce the problem to a single, ordinary differential equation for the evolution function. In general, two regimes of evolution are possible; expansion and oscillation. We investigate the specific effect rotation has on these two modes of evolution. We focus on critical values of the flux rope parameters and show that rotation can suppress the oscillatory mode. We estimate the critical value of the angular velocity _crit, above which the magnetic flux rope always expands, regardless of the value of the initial energy. Studying small-amplitude oscillations of the rope, we find that torsional oscillations are superimposed on the rotation and that they have a frequency equal to that of the radial oscillations. By setting the axial component of the magnetic field to zero, we study small-amplitude oscillations of a rigidly rotating pinch. We find that the frequency of oscillation is inversely proportional to the angular velocity of rotation ; the product being proportional to the inverse square of the Alfvén time. The period of large-amplitude oscillations of a rotating flux rope of low beta increases exponentially with the energy of the equivalent 1D oscillator. With respect to large-amplitude oscillations of a non-rotating flux rope, the only change brought about by rotation is to introduce a multiplicative factor greater than unity, which further increases the period. This multiplicative factor depends on the ratio of the azimuthal speed to the Alfvén speed. Finally, considering interplanetary magnetic clouds as cylindrical flux ropes, we inquire whether they rotate. We find that at 1 AU only a minority do. We discuss data on two magnetic clouds where we interpret the presence in each of vortical plasma motion about the symmetry axis as a sign of rotation. Our estimates for the angular velocities suggest that the parameters of the two magnetic clouds are below critical values. The two clouds differ in many respects (such as age, bulk flow speed, size, handedness of the magnetic field, etc.), and we find that their rotational parameters reflect some of these differences, particularly the difference in age. In both clouds, a rough estimate of the radial electric field in the rigidly rotating core, calculated in a non-rotating frame, yields values of the order mV m⁻¹.     

Resistive instabilities in rapidly rotating fluids: Linear theory of the convective modes

Abstract

This paper analyzes the linear stability of a rapidly-rotating, stratified sheet pinch in a gravitational field, g, perpendicular to the sheet. The sheet pinch is a layer (O ? z ? d) of inviscid, Boussinesq fluid of electrical conductivity σ, magnetic permeability μ, and almost uniform density ρ _o; z is height. The prevailing magnetic field. B _o(z), is horizontal at each z level, but varies in direction with z. The angular velocity, Ω, is vertical and large (Ω ? V_A/d, where V_A = B₀√(μρ₀) is the Alfvén velocity). The Elsasser number, Λ = σB² ₀/2Ωρ₀, measures σ. A (modified) Rayleigh number, R = gβd²/ρ₀V² _A, measures the buoyancy force, where β is the imposed density gradient, antiparallel to g. A Prandtl number, P_K = μσK, measures the diffusivity, k, of density differences.     

颈动脉粥样硬化斑块与急性缺血性脑卒中的相关性研究

目的：运用颈动脉CTA分析颈动脉粥样硬化斑块,探讨斑块性质及部分因素与急性缺血性脑卒中的相关性,从而为急性缺血性脑卒中的预防和治疗提供参考和依据。方法：回顾性分析行颈动脉CTA检查、且在颈动脉CTA检查前或后一周内行磁共振DWI检查的患者,根据磁共振DWI判断有无前循环急性缺血性脑卒中,将患者分为急性缺血性脑卒中组（95例）和非急性缺血性脑卒中组（102例）;对两组患者的临床资料、实验室资料和CTA显示的颈动脉斑块性质、斑块表面形态进行分析,比较两组之间有无统计学差异,对P <0.05的指标纳入急性缺血性脑卒中发生的多因素Logistic回归分析。结果：两组间在年龄、高血压病史、TC、TG、HDL、HCY、CysC、HbA1c指标中差异有统计学意义;两组间在斑块性质及斑块表面形态间差异有统计学意义,在颈动脉管腔狭窄程度间差异无统计学意义;多因素回归分析提示年龄≥65岁、高血压、TC、HDL、HCY及脂质斑块是急性缺血性脑卒中发生的危险因素。结论：颈动脉粥样硬化与急性缺血性脑卒中发生相关,脂质斑块是急性缺血性脑卒中发生的危险因素;颈动脉CTA可以对斑块性质进行判断,结合部分实验室指...     

无源自适应磁流变阻尼器设计与研究

针对防震、航空航天、野战军械等领域对能源的限制,以及车辆减振中对阻尼器拉压行程不同阻尼力大小的要求,设计制作了一个无源自适应磁流变阻尼器。该阻尼器采用磁致伸缩逆效应及磁流变液的特性,把负载力的变化转化为磁流变液间隙处磁场的变化,解决了常规的磁流变阻尼器需要外配能源装置及控制电路的问题。对该阻尼器进行了建模,并进行了阻尼特性试验,结果表明:试验数据与模型符合得较好,阻尼力大小和负载有关,拉力越大,阻尼力越大,压力越大,阻尼力越小,具有负载自适应的特点,验证了设计的可行性。     

金属套管对多分量电磁感应测井信号的影响

研究金属套管对低频电磁场各分量透射信号和反射信号的影响规律对采用过套管电磁感应测井技术监测生产过程中的流体移动具有重要价值.采用柱状成层各向异性介质中的并矢Green函数模拟当发射源在套管内、接收器分别在套管内和套管外时多分量电磁感应的响应,并系统分析了金属套管对透射磁场和反射磁场各主分量的影响规律.计算结果表明,无论是透射场还是反射场,由于所采用的频率较低,金属套管对每个分量信号的影响可以与地层对该分量信号的影响分开.在低频段,磁性金属套管对磁场各分量仍存在稳定的反射,但不同分量被反射的程度不同,受套管磁屏蔽作用大的分量(如ρρ分量)被反射的程度高于受套管磁屏蔽作用小的分量(如zz分量).随着频率的升高,反射磁场的强度逐渐增大并最终达到饱和,信号被全反射.磁性金属套管的存在导致透射磁场各分量出现不同程度的幅度衰减和相位延迟,受套管磁屏蔽作用大的分量的幅度衰减程度大.在固定套管参数和频率的情况下,磁性套管对透射磁场不同分量的影响程度虽然不同但是恒定,其所导致的各分量的幅度衰减和相位延迟与线圈系位置和地层电参数无关.在低频段,套管外透射场的各分量处于准静态,其幅度和相位均不随频率而改变,受套管磁屏蔽作用大的分量的幅度随套管磁导率和厚度的不同而存在明显变化.当频率超过某一临界值后,套管的影响逐渐从以静态屏蔽为主转到以趋肤效应为主,导致透射场幅度的衰减和相位的延迟,套管的厚度越大、套管的电导率和相对磁导率值越大,所对应的频率临界值越小.     

Compressible Ekman–Hartmann boundary layers

We consider the effect of compressibility on mixed Ekman–Hartmann boundary layers on an infinite plane (z = 0), in the presence of an external magnetic field oblique to the boundary. The aim is to investigate the influence of the magnetic pressure on the fluid density, and hence, via mass conservation, on the mass flow into or out of the boundary layer. We find that if the z-component of vorticity in the main flow, immediately above the boundary layer, is negative, then there is a competition between Ekman suction and the magnetic pressure effect. Indeed, as the magnetic field strength is increased, the magnetic pumping may overcome the Ekman suction produced by anti-cyclonic main flow vortices. Such a mechanism, based on the competition between these effects, may be of importance for understanding the dynamics of the magnetic field in stellar (or planetary) interiors. For the solar tachocline, we find that the analysed magnetic pressure effect is unlikely to play a significant role; however, we give examples of what changes in the assumed scalings would be necessary for the effect to become important.     

改进磁变仪布局的研究

本文讨论了各分量磁变仪磁针之间的相互影响以及地磁场各分量的变化、记录光入射角对记录的影响，并由此认为一套磁变仪的布局应满意三项标准：（１）各分量仪磁针间的相互静磁影响要小，且任一磁针受其它磁针工作的影响要低于该分量仪记录的分辨率；（２）各分量仪的状态函数稳定，即保持定向能力强；（３）可产生较高精度的线性记录磁照图。鉴于目前的磁变仪布局与此三标准有明显差距，故本文提出了一种新的布局方案，可满足此三项     

The effects of particle breakage and abrasion on the magnetic properties of two soils

As mineral magnetism is used as a tracer for sourcing river and dam sediments, changes in the magnetic properties that may occur during transport between the source and sink must be considered. Abrasion and breakage of particles will occur during transport. These processes were examined in simulation experiments with a granitic and a sedimentary soil. The effects of these processes on the magnetic properties of a granitic and a sedimentary soil were examined using a simulated breakage/abrasion experiment. Breakage and/or abrasion had substantial effects on the magnetic properties of both soils. All particle sizes were affected, but the magnitude varied through the size range of derived particles. The major effect was on the concentration of magnetic minerals, with differences between the concentrations in particle sizes of the original material and those generated by the experiments being as much as 20 times. The effect on the granite soil was to reduce the concentrations, i.e. derived material was less than original material; whereas for the sedimentary soil the derived particles had higher concentrations. The effect on magnetic grain size, as indicated by the magnetic ratios, was less than the effect on the mass magnetic properties, but still substantial for some ratios for some sizes. © 1998 John Wiley & Sons, Ltd.     

Numerical simulations of MHD dynamos

The generation of magnetic fields in space plasmas and in astrophysics is usually described within the framework of magnetohydrodynamics. Turbulent helical flows produce magnetic fields very efficiently, with correlation length scales larger than those characterizing the flow. Within the context of the solar magnetic cycle, a turbulent dynamo is responsible for the so-called alpha effect, while the Omega effect is associated to the differential rotation of the Sun.We present direct numerical simulations of turbulent magnetohydrodynamic dynamos including two-fluid effects such as the Hall current. More specifically, we study the evolution of an initially weak and small-scale magnetic field in a system maintained in a stationary regime of hydrodynamic turbulence, and explore the conditions for exponential growth of the magnetic energy. In all the cases considered, we find that the dynamo saturates at the equipartition level between kinetic and magnetic energy, and the total energy reaches a Kolmogorov power spectrum.     

Scaling Law for Galactic Magnetic Fields

A nonlinear mean field dynamo in turbulent disks and spherical shells is discussed. We use a nonlinearity in the dynamo which includes the effect of delayed back-reaction of the mean magnetic field on the magnetic part of the — effect. This effect is determined by an evolutionary equation. The axisymmetric case is considered. An analytical expression (in a single-mode approximation) is derived which gives the magnitude of the mean magnetic field as a function of rotation and the parameters for turbulent disks. The value obtained for the mean magnetic field is in agreement with observations for galaxies.     

Mechanisms of conversion of kinetic into magnetic energy in partially ionized plasmas

The processes involved in the transformation of kinetic into magnetic energy in partially ionized compressible plasmas are not limited to the well-known mechanism of transport and diffusion of single-fluid magnetohydrodynamics. The induction equation, in this new case, may be written for any mean of the ion and electron velocities, and it possesses a natural scaling parameter equal to the ratio of the electron and ion masses. This produces a hierarchy of sources able to generate a magnetic field. The first of these sources corresponds to the classical stretching of magnetic field lines by the flow and ohmic diffusion, and a compressional effect due to the flow of electromagnetic energy into the regions of higher density. A potentially important effect is caused by dragging of electrons by neutral particles through collisions; this term could dissipate as well as enhance the magnetic field depending on the geometry of the neutral flow. Finally, there exists a term analogous to the stretching one, this time involving the current density and with the opposite effect. Its presence implies that not only the magnetic field but also the current density grows at most exponentially with a growth rate bounded by the maximum of the strain matrix. While the effect of these nonclassical sources, acting alone, is in all probability extremely small, they could be relevant in the creation of seed magnetic fields for subsequent dynamo action.     

钢筋混凝土核心简的剪切滞变模型

通过对比评价现有可用于剪力墙的剪切滞变模型,并结合现有国内外钢筋混凝土核心筒体试验结果,选取了带捏缩的修正Takeda模型作为核心筒的剪切滞变模型,并给出了模型的细部滞变规则。     

Fast damping of acoustic waves in solar coronal loops as a result of their radiation

The problem of the observed fast damping of longitudinal waves in solar coronal magnetic loops is studied. According to some data, the radiation effect, which plays a key role in the cooling of coronal loops that are observed in the extreme UV wavelength range, is used to explain this phenomenon. The dispersion relation for slow magnetosonic modes of a cylindrical magnetic tube has been obtained with regard to the radiation effect. It has been indicated that the radiation actually results in the fast damping of the slow magnetosonic modes of coronal magnetic loops.     

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.     

方钢管混凝土压弯构件滞回性能的试验研究

以轴压比和含钢率为试验参数，进行了7个方面钢管混凝土压弯构件在往复荷载作用下荷载－位移滞回性能的试验研究，所得滞回曲线的图形都具有较好的饱满性，且和数值计算结构吻合良好，还利用已有的恢复力对构件进行了滞回曲线的理论计算，并和试验结果进行了分析对比，结果表明二者基本吻合。     

Electromagnetic Methods of Lightning Detection

Both cloud-to-ground and cloud lightning discharges involve a number of processes that produce electromagnetic field signatures in different regions of the spectrum. Salient characteristics of measured wideband electric and magnetic fields generated by various lightning processes at distances ranging from tens to a few hundreds of kilometers (when at least the initial part of the signal is essentially radiation while being not influenced by ionospheric reflections) are reviewed. An overview of the various lightning locating techniques, including magnetic direction finding, time-of-arrival technique, and interferometry, is given. Lightning location on global scale, when radio-frequency electromagnetic signals are dominated by ionospheric reflections, is also considered. Lightning locating system performance characteristics, including flash and stroke detection efficiencies, percentage of misclassified events, location accuracy, and peak current estimation errors, are discussed. Both cloud and cloud-to-ground flashes are considered. Representative examples of modern lightning locating systems are reviewed. Besides general characterization of each system, the available information on its performance characteristics is given with emphasis on those based on formal ground-truth studies published in the peer-reviewed literature.     

Palaeomagnetic distortion modelling and possible recovery by inversion

A robust finite-element technique is presented for computation of both the internal demagnetization effects and magnetic terrain effects in bodies with arbitrary shape and arbitrary susceptibility distribution. This method facilitates a flexible analysis of the palaeomagnetic deflection problem. Tests on geologically realistic settings of highly magnetic rocks demonstrate that deflections of several degrees may occur even for relatively simple two-dimensional models. Similarly, the magnetic intensity may well be biased by 5-15% by demagnetization effects. The present paper focuses on deflections and intensity variations inside the magnetized body, where we find a systematic shallowing of inclination for bodies with a horizontal elongation. Because the bodies sampled at a typical palaeomagnetic site will have a dominant direction of elongation, the magnetic deflection effect will tend to impose a systematic bias which doesn’t average out. An inversion-based procedure for elimination of the deflection effect is presented. It requires that the magnetic body is quite homogeneous and that its surface geometry is known, as may be the case for historical lava flows. Tests demonstrate that in order to recover both ambient palaeofield direction and the effective susceptibility at blocking temperature it is necessary to sample near strong topographic elements in the magnetic body. Since the surface geometry rarely is known it is proposed as an alternative to inversion that an effective susceptibility is assessed and a horizontal slab correction is applied for samples taken far from topographical features. When shape geometry is unknown and no correction applied, palaeomagnetic conclusions must take into account the possible bias from internal demagnetization and magnetic terrain effects.     

A note on magnetic modelling with remanence

The general problem of magnetic modelling involves accounting for the effect of both remanent magnetization and the application of an external magnetic field. However, as far as the disturbing field of a magnetic body in a magnetic environment is concerned, there is an equivalence between the effects of these two causations that allows the remanence to be represented in terms of an equivalent primary magnetic H field. Moreover, due to the linearity of the magnetic field in terms of its causations, the general modelling problem involving an applied magnetic field in the presence of remanence can be simply and more efficiently dealt with in terms of an equivalent primary field acting in the absence of any remanent magnetization.     

Shear flow instability of rotating hydromagnetic fluids

Abstract

The effect of an axial magnetic field on the linear stability of shear flows in rotating systems is examined by extending Busse's analysis of the nonmagnetic case to fluids of high magnetic diffusivity in the presence of a magnetic field. The shear is caused by differential rotation which creates slight deviations from a state of rigid rotation, corresponding to a small Rossby number. It is found that the Rossby number for the onset of instability is larger when a magnetic field is present than when it is absent.