Asymmetric magnetic field inside a cylindrical flux rope

In order to consider an asymmetric field distribution inside a cylindrical tube with a circular cross section, with the field magnitude maximum reached at a point different from the geometrical centre of the tube, we propose a new solution obtained in bi-cylindrical coordinates. If the parameter of the system is very large, the solution approaches the well known symmetric Lundquist solution. The new solution models a field magnitude shift due to relative motion of the cylinder and the ambient solar wind. If the cylinder is moving much faster than the ambient medium, its field maximum is shifted forward, otherwise it is shifted in the opposite direction.     

带LCD复位的正—反激组合式变换器的理论分析与实验验证

正－反激组合式变换器中，两个变压器轮流向负载传递功率，ＬＣＤ缓冲网络实现了功率器件的零电压关断，并且将多余的能量回馈电网，减小了关断损耗，提高了效率，文中详细分析了该变换器的工作原理，列出了各种工作状态下的等值电路和微分方程，给出了各工作状态转换的条件，并绘制了５０Ｗ１００ｋＨｚ实验电路的实验波形，验证了理论分析的正确性。     

On the Origin of the Strong Intermittent Nature of Interplanetary Magnetic Field

We briefly discuss the strong intermittent nature of the interplanetary magnetic field, observing that similarity between its statistical properties and the passive scalar ones exists, and may arise from different dynamical mechanisms.     

基于MATLAB下的磁性测量新方法

在简单介绍磁性测量冲击法基本原理的基础上,提出了一种将多元回归分析应用于磁性测量中的新方法。着重讲述了如何实现基于多元回归分析法下的磁性测量新方法,借助于MATLAB语言编辑可实现多元回归算法及磁测新方法的多个可嵌套调用的GUI界面。实践证明,使用MATLAB可实现磁性测量新方法,该方法大大缩短了测量周期,所编辑的GUI界面充分利用了MATLAB函数库,可快速精确的处理磁测数据,建立回归模型,保存并显示计算结果,且操作方便。     

Solar Wind Control of the Magnetospheric and Auroral Dynamics

A dependence of the polar cap magnetic flux on the interplanetary magnetic field and on the solar wind dynamic pressure is studied. The model calculations of the polar cap and auroral oval magnetic fluxes at the ionospheric level are presented. The obtained functions are based on the paraboloid magnetospheric model calculations. The scaling law for the polar cap diameter changing for different subsolar distances is demonstrated. Quiet conditions are used to compare theoretical results with the UV images of the Earth’s polar region obtained onboard the Polar and IMAGE spacecrafts. The model calculations enable finding not only the average polar cap magnetic flux but also the extreme values of the polar cap and auroral oval magnetic fluxes. These values can be attained in the course of the severe magnetic storm. Spectacular aurora often can be seen at midlatitude during severe magnetic storm. In particularly, the Bastille Day storm of July 15–16, 2000, was a severe magnetic storm when auroral displays were reported at midlatitudes. Enhancement of global magnetospheric current systems (ring current and tail current) and corresponding reconstruction of the magnetospheric structure is a reason for the equatorward displacement of the auroral zone. But at the start of the studied event the contracted polar cap and auroral oval were observed. In this case, the sudden solar wind pressure pulse was associated with a simultaneous northward IMF turning. Such IMF and solar wind pressure behavior is a cause of the observed aurora dynamics.     

The solar wind control of the equatorial ionosphere dynamics during geomagnetic storms

The interplanetary magnetic field, geomagnetic variations, virtual ionosphere height h′F, and the critical frequency foF2 data during the geomagnetic storms are studied to demonstrate relationships between these phenomena. We study 5-min ionospheric variations using the first Western Pacific Ionosphere Campaign (1998–1999) observations, 5-min interplanetary magnetic field (IMF) and 5-min auroral electrojets data during a moderate geomagnetic storm. These data allowed us to demonstrate that the auroral and the equatorial ionospheric phenomena are developed practically simultaneously. Hourly average of the ionospheric foF2 and h′F variations at near equatorial stations during a similar storm show the same behavior. We suppose this is due to interaction between electric fields of the auroral and the equatorial ionosphere during geomagnetic storms. It is shown that the low-latitude ionosphere dynamics during these moderate storms was defined by the southward direction of the B_z-component of the interplanetary magnetic field. A southward IMF produces the Region I and Region II field-aligned currents (FAC) and polar electrojet current systems. We assume that the short-term ionospheric variations during geomagnetic storms can be explained mainly by the electric field of the FAC. The electric fields of the field-aligned currents can penetrate throughout the mid-latitude ionosphere to the equator and may serve as a coupling agent between the auroral and the equatorial ionosphere.     

Mode selection mechanism and magnetic diffusivity in a non-axisymmetric solar dynamo model

The generation of solar non-axisymmetric magnetic fields is studied based on a linear α²–Ω dynamo model in a rotating spherical frame. The model consists of a solar-like differential rotation, a magnetic diffusivity varied with depth, and three types of α-effects with different locations, i.e. the tachocline, the whole convective zone and the sub-surface. Some comparisons of the critical α-values of axisymmetric (m = 0) and longitude-dependent modes (m = 1,2,3) are presented to show the roles of the magnetic diffusivity in the problem of modes selection. With the changing of diffusivity intensity for the given solar differential rotation system, the dominant mode possibly changes likewise and the stronger the diffusivity is, the easier the non-axisymmetric modes are excited. The influence of the diffusivity and differential rotation on the configurations of the dominant modes are also presented.     

Diagnosis of coronal magnetic field and nonthermal electrons from Nobeyama observations of a simple flare

Coronal magnetic field and nonthermal electrons are very important parameters for understanding of the global heliophysical processes. A flare on November 1, 2004 is selected for self-consistent calculations of coronal magnetic field parallel and perpendicular to the line-of-sight, and density of nonthermal electrons from Nobeyama observations. Both of the diagnosis methods and results are discussed in this paper.     

How far are we from a ‘Standard Model’ of the solar dynamo?

Over the last few years, dynamo theorists seem to be converging on a basic scenario as to how the solar dynamo operates. The strong toroidal component of the magnetic field is produced in the tachocline, from where it rises due to magnetic buoyancy to produce active regions at the solar surface. The decay of tilted bipolar active regions at the surface gives rise to the poloidal component, which is first advected poleward by the meridional circulation and then taken below the surface to the tachocline where it can be stretched to produce the toroidal component. The mathematical formulation of this basic model, however, involves the specification of some parameters which are still uncertain. We review these remaining uncertainties which have resulted in disagreements amongst various research groups and have made it impossible to still arrive at something that can be called a standard model of the solar dynamo.     

The Solar Magnetic Field as a Coronal Hole Extension Forms: Effects of Magnetic Helicity and Boundary Conditions

An analytical solution is presented for linear force fields within a spherical shell, representing the solar corona. Allowing for a global magnetic helicity, we find magnetic fields over the entire corona with realistic inner boundary conditions obtained from transformation and extrapolation of photospheric magnetograms and considering alternative outer boundary conditions. Such fields are found for the well known coronal hole extension event of August 1996. This revised version was published online in June 2006 with corrections to the Cover Date.