Theoretical Advances in Prominence Seismology

Prominence seismology is a rapidly developing topic which seeks to infer the internal structure and properties of solar prominences from the study of its oscillations. An extensive observational background about oscillations in quiescent solar prominences has been gathered during the last 70 years. These observations point out the existence of two different types of oscillations: Flare-induced oscillations (winking filaments) which affect the whole prominence and are of large amplitude and small amplitude oscillations which seem to be of local nature. From the theoretical point of view, few models have been set up to explain the phenomenon of winking filaments while, on the contrary, for small amplitude oscillations a large number of models trying to explain the observed features have been proposed.     

Standing Slow-Mode Waves in Hot Coronal Loops: Observations, Modeling, and Coronal Seismology

Strongly damped Doppler shift oscillations are observed frequently associated with flarelike events in hot coronal loops. In this paper, a review of the observed properties and the theoretical modeling is presented. Statistical measurements of physical parameters (period, decay time, and amplitude) have been obtained based on a large number of events observed by SOHO/SUMER and Yohkoh/BCS. Several pieces of evidence are found to support their interpretation in terms of the fundamental standing longitudinal slow mode. The high excitation rate of these oscillations in small- or micro-flares suggest that the slow mode waves are a natural response of the coronal plasma to impulsive heating in closed magnetic structure. The strong damping and the rapid excitation of the observed waves are two major aspects of the waves that are poorly understood, and are the main subject of theoretical modelling. The slow waves are found mainly damped by thermal conduction and viscosity in hot coronal loops. The mode coupling seems to play an important role in rapid excitation of the standing slow mode. Several seismology applications such as determination of the magnetic field, temperature, and density in coronal loops are demonstrated. Further, some open issues are discussed.     

MHD structures, waves and turbulence in the solar wind: Observations and theories

A comprehensive overview is presented of recent observational and theoretical results on solar wind structures and fluctuations and magnetohydrodynamic waves and turbulence, with preference given to phenomena in the inner heliosphere. Emphasis is placed on the progress made in the past decade in the understanding of the nature and origin of especially small-scale, compressible and incompressible fluctuations. Turbulence models to describe the spatial transport and spectral transfer of the fluctuations in the inner heliosphere are discussed, and results from direct numerical simulations are dealt with. Intermittency of solar wind fluctuations and their statistical distributions are briefly investigated. Studies of the heating and acceleration effects of the turbulence on the background wind are critically surveyed. Finally, open questions concerning the origin, nature and evolution of the fluctuations are listed, and possible avenues and perspectives for future research are outlined.     

磁射流抛光中磁场的分析与设计

介绍了一种新型抛光技术——磁射流抛光中磁场对磁流变液粘度的影响,设计了相适应的磁场形式,重点分析了铁磁喷嘴头部形状对磁场的影响,并通过ANSYS有限元软件仿真了结构形状对磁场空间特性的影响。     

Theory and Simulation of Reconnection

Reconnection is a major commonality of solar and magnetospheric physics. It was conjectured by Giovanelli in 1946 to explain particle acceleration in solar flares near magnetic neutral points. Since than it has been broadly applied in space physics including magnetospheric physics. In a special way this is due to Harry Petschek, who in 1994 published his ground breaking solution for a 2D magnetized plasma flow in regions containing singularities of vanishing magnetic field. Petschek’s reconnection theory was questioned in endless disputes and arguments, but his work stimulated the further investigation of this phenomenon like no other. However, there are questions left open. We consider two of them – “anomalous” resistivity in collisionless space plasma and the nature of reconnection in three dimensions. The CLUSTER and SOHO missions address these two aspects of reconnection in a complementary way -- the resistivity problem in situ in the magnetosphere and the 3D aspect by remote sensing of the Sun. We demonstrate that the search for answers to both questions leads beyond the applicability of analytical theories and that appropriate numerical approaches are necessary to investigate the essentially nonlinear and nonlocal processes involved. Necessary are both micro-physical, kinetic Vlasov-equation based methods of investigation as well as large scale (MHD) simulations to obtain the geometry and topology of the acting fields and flows.     

原子磁力仪的空间应用及发展趋势

在太空探索中,磁场测量为很多重要的科学研究提供了数据支撑。空间探测器和磁测卫星均多次采用原子磁力仪作为磁场测量的主载荷,原子磁力仪在空间磁场测量中发挥着不可替代的作用。回顾了用于空间磁场测量的原子磁力仪的发展历程,总结了不同种类原子磁力仪的技术特点,分析了空间应用原子磁力仪载荷的发展趋势。     

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.     

On the Velocity and Intensity Asymmetries of Solar P-Mode Lines

We show that to explain the opposite line asymmetries shown by the velocity and intensity spectra, it is necessary to solve the full non-adiabatic problem which is at least of the fourth order. This revised version was published online in June 2006 with corrections to the Cover Date.     

非导磁不锈钢管材内外表面的磁力研磨

针对非导磁材料难以采用磁力研磨的问题,本文研制了特定的磁路,磁极表面场强达8kGOs以上,并成功地对3mm壁厚的不锈钢管材的内外表面进行了磁力研磨,尤其是外表面磁力研磨后表面粗糙度达0.06μm。     

任意形状平面载流线圈在远点处的磁场计算

在电磁场中,经常计算圆环、矩形、三角形等规则平面载流线圈特殊点（如中心轴线上）的磁场分布规律,而复杂一些的问题,例如规则平面载流线圈的远点和任意点的磁场分布规律由于数学处理繁杂一般不加以计算.实践中通过对规则平面载流线圈中心轴线上任意一点和与该线圈共面的对称线上的任意一点的磁场分布规律的整理分析,用二者合成的方法,经推广得出一般性规律,可以解决任意形状的平面载流线圈在远点处这一类的磁场计算问题.     

三轴矢量原子磁力仪综述

原子磁力仪可分为标量磁力仪和矢量磁力仪两大类。标量磁力仪的测量结果与传感器的姿态无关,对平台的机动不敏感。矢量磁力仪能够获得更多的磁场信息,可以实现更精确的磁源定位。目前,共有7种三轴矢量原子磁力仪,测量方法分别为磁场扫描法、磁场旋转调制法、磁场轮流抵消法、磁场投影法、磁场交叉调制法、磁场分立调制法和自旋进动调制法。重点对上述7种三轴矢量原子磁力仪的测量方法进行了整理和分析。     

一维钡铁氧体纳米线的制备及操控

采用Sol-gel法,以自制的AAO模板制备了直径40～60nm,长度为150～200nm的一维BaFe12O19纳米线.利用X射线衍射(XRD),场发射扫描电镜(FESEM),振动样品磁强计(VSM)对BaFe12O19纳米线的组成、形貌与磁性能进行了研究.在外磁场的驱动下,对一维BaFe12O19纳米线进行操控.研究发现:BaFe12O19纳米线的易磁化方向平行其轴线方向,且操控后,BaFe12O19纳米线定向连接成“链”,当磁场与BaFe12O19纳米链阵列平行(∥)时,纳米链的剩余磁化强度(Mr)、饱和磁化强度(Ms)和最大磁能积(BH)m都得到增强.矫顽力(He)由3.98×105A/m增大至5.01×105 A/m,矩形比为0.9,可成为优异的高密度垂直磁记录材料.     

Coronal Heating by Magnetic Explosions

From magnetic fields and coronal heating observed in flares, active regions, quiet regions, and coronal holes, we propose that exploding sheared core magnetic fields are the drivers of most of the dynamics and heating of the solar atmosphere, ranging from the largest and most powerful coronal mass ejections and flares, to the vigorous microflaring and coronal heating in active regions, to a multitude of fine-scale explosive events in the magnetic network, driving microflares, spicules, global coronal heating, and, consequently, the solar wind. This revised version was published online in June 2006 with corrections to the Cover Date.     

Microwave Diagnostics of Dynamic Processes and Oscillations in Groups of Solar Coronal Magnetic Loops

Low-frequency (LF) modulations of the solar microwave radiation (37 GHz) recorded at the Metsähovi Radio Observatory, are analyzed. Since the intensity of solar microwave radiation, produced by the electron gyrosynchrotron mechanism, is dependent on a value of the background magnetic field [Dulk, G. A.: 1985, Ann. Rev. Astron. Astrophys. 23, 169–224], slow variations of the magnetic field associated with disturbances of the electric current in a radiating source, can modulate the intensity of the microwave radiation. The observed multi-track features of the LF spectra are interpreted as a signature of a complex multi-loop structure of the radiating source. Application of the equivalent electric circuit models of interacting loops allows to explain and reproduce the main dynamical features of the observed LF modulation dynamic spectra.     

电子回旋共振中和器内静磁场及微波电磁场的数值计算

为了研究电子回旋共振中和器内静磁场和微波电磁场的分布规律,设计合理的磁路结构以形成电子回旋共振区,并使微波强电场区与电子回旋共振区重合,采用有限元分析软件对中和器内的静磁场和微波电磁场进行了数值计算。计算结果表明:永磁体及磁轭的尺寸均影响电子回旋共振区的分布;天线伸入长度越长,微波电场越强。微波频率为4.2GHz时,六块相同的长12mm,宽8mm,高5mm的条形永磁铁与磁轭组成的磁路结构,可以产生合理的电子回旋共振区。L型天线伸入长度为5mm时微波强电场区可与电子回旋共振区重合。     

The Strength and Structure of the Coronal Magnetic Field

I discuss a method for determining the strength and spatial structure of the coronal magnetic field by observations of the Faraday rotation of a radio galaxy which is in conjunction with the Sun. Given a knowledge of the plasma density in the outer corona, and the magnetic field sector structure (both independently available), the strength of the coronal field can be determined, as well as the magnitude of spatial variations on scales of 1000 km to several solar radii. Such knowledge is crucial for testing computational models of the solar corona, which are prominently featured in this meeting. Results are presented from observations with the Very Large Array radio telescope of the radio galaxy 3C228 on August 16, 2003, when the line of sight to the source was at heliocentic distances of 7.1−6.2R _⊙. The observations are consistent with a coronal magnetic field which is proportional to the inverse square of the distance in the range 6 ≤ r ≤ 10R _⊙, and has a value of 39 mG at 6.2R _⊙. The Faraday rotation is uniform across the source, indicating an absence of strong plasma inhomogeneity on spatial scales up to 35,000 km.     

几种新的单路原子磁导引磁场设计和分析

原子磁导引利用载流导线产生的磁场与原子相互作用来操控冷原子,针对冷原子操控和传输的要求,提出了双曲线薄板导引、双平行平板导引、三根等边三角形和四根正方形分布载流导线实现对冷原子进行单路磁导引的方案,利用Ansoft maxwell 2D软件计算各导引的磁场分布和沿特殊轴的磁场变化值,分析其导引特点。这几种磁导引都采用通直流电的载流导体,其结构中心位置的场强存在极小值,形成了沿着导引的方向呈现管状磁场分布,适合导引弱场搜寻态的原子。越接近导体表面的地方,磁场梯度越大,所以原子不易与材料的相互作用而被吸引到导体表面造成损耗,而且使用时不需另加控制磁场,在实验中易于实现。     

Observations of the local interstellar medium with the Extreme Ultraviolet Explorer

Because of the strong absorption of extreme ultraviolet radiation by hydrogen and helium, almost every observation with the Extreme Ultraviolet Explorer (EUVE) satellite is affected by the diffuse clouds of neutral gas in the local interstellar medium (LISM). This paper reviews some of the highlights of the EUVE results on the distribution and physical state of the LISM and the implications of these results with respect to the interface of the LISM and the heliosphere. The distribution of sources found with the EUVE all-sky surveys shows an enhancement in absorption toward the galactic center. Individual spectra toward nearby continuum sources provide evidence of a greater ionization of helium than hydrogen in the Local Cloud with an mean ratio of H I/He I of 14.7. The spectral distribution of the EUV stellar radiation field has been measured, which provides a lower limit to local H II and He II densities, but this radiation field alone cannot explain the local helium ionization. A combination of EUVE measurements of H I, He I, and He II columns plus the measurement of the local He I density with interplanetary probes can place constraints on the local values of the H I density outside the heliosphere to lie between 0.15 and 0.34 cm^–3 while the H II density ranges between 0.0 and 0.14 cm^–3. The thermal pressure (P/k = nT) of the Local Cloud is derived to be between 1700 and 2300 cm^–3 K, a factor of 2 to 3 above previous estimates.     

An Introduction to the Pre-CME Corona

Coronal mass ejections provide a gateway to understanding the physics of energy release and conversion in the solar corona. While it is generally accepted that the energy required to power a CME is contained in the pre-eruption coronal magnetic field, the pre-CME state of that field and the conditions leading up to the release of the magnetic energy are still not entirely clear. Recent studies point to various phenomena which are common to many, if not all, CME events, suggesting that there may be identifiable characteristics of the pre-CME corona which signal the impending eruption. However, determining whether these phenomena are necessary or even sufficient has yet to be achieved. In this paper we attempt to summarize the state of the solar corona and its evolution in the build up to a CME.