Seismology of Prominence-Fine structures: Observations and Theory

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. Two-dimensional high-resolution observations suggest that filaments can be considered as made by small scale fibrils, having a cool region, stacked one after another in the vertical and horizontal directions. An extense observational background about oscillations in filaments has been gathered during the last 20 years and these observations point out that fibrils or groups of fibrils can oscillate independently. From the theoretical point of view, small amplitude oscillations in single and multifibril configurations have been studied as a first step to explain observational features.     

核磁共振陀螺中静磁场强度对原子核自旋进动信号的影响

原子核自旋磁矩Larmor进动达到稳态时,检测光携带出的信息中同时包含原子核自旋进动磁场信号和驱动磁场信号,且这两种磁场信号的幅值比例会随静磁场强度改变发生显著变化.从理论和实验两方面研究了检测信号中原子核自旋进动磁场与驱动磁场的比例关系,通过分析不同静磁场下的弛豫信号幅值变化,发现静磁场能够显著抑制驱动磁场对原子核自...     

Energy release in stellar magnetospheres

The interaction of a stellar magnetosphere with a thin accretion disk is considered. Specifically, I consider a model in which (1) the accretion disk is magnetically linked to the star over a large range of radii and (2) the magnetic diffusivity of the disk is sufficiently small that there is little slippage of field lines within the disk on the rotation time scale. In this case the magnetic energy built up as a result of differential rotation between the star and the disk is released in quasi-periodic reconnection events occuring in the magnetosphere (Aly and Kuijpers 1990). The radial transport of magnetic flux in such an accretion disk is considered. It is show that the magnetic flux distribution is stationary on the accretion time scale, provided the time average of the radial component of the field just above the disk vanishes. A simple model of the time-dependent structure of the magnetosphere is presented. It is shown that energy release in the magnetosphere must take place for (differential) rotation angles less than about 3 radians. The magnetic flux distribution in the disk depends on the precise value of the rotation angle.     

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。     

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.     

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.     

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.     

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。     

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.     

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.     

高灵敏度与高稳定性的飞机客舱内物品监测系统

介绍了一种新型的高稳定度、高灵敏度的飞机客舱内物品监测系统的工作原理和基本电路。该系统具有检测灵敏度高,抗干扰能力强,工作稳定可靠的特点。     

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.     

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。     

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。     

磁场作用下的TIG电弧行为分析

在磁流体动力学理论的基础上,针对外加纵向磁场作用下的钨极氩弧焊(TIG)电弧在旋转圆柱坐标系中建立了不同电流密度的数学模型.通过Fluent用户自定义函数进行编程开发,对其流场和电磁场进行耦合求解,得到了外加纵向磁场作用下的TIG电弧热场和流场的分布规律.结果 表明,纵向磁场作用下的TIG电孤温度场呈现空心钟罩形态,并...     

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。     

核磁共振陀螺仪中共振磁场强度优化研究

核磁共振陀螺中,共振磁场的幅值直接影响原子核自旋磁矩进动信号的强度,进而影响陀螺信号的信噪比.基于核磁共振陀螺Bloch方程,从理论和实验两方面研究了共振磁场幅值对宏观原子核自旋磁矩的影响.结果表明,随着共振磁场幅值的增加,宏观核自旋磁矩进动信号的强度先增大后减小,进动信号的强度与共振磁场的幅值呈色散关系.共振磁场幅度...     

The Origin of Mercury’s Internal Magnetic Field

Mariner 10 measurements proved the existence of a large-scale internal magnetic field on Mercury. The observed field amplitude, however, is too weak to be compatible with typical convective planetary dynamos. The Lorentz force based on an extrapolation of Mariner 10 data to the dynamo region is 10⁻⁴ times smaller than the Coriolis force. This is at odds with the idea that planetary dynamos are thought to work in the so-called magnetostrophic regime, where Coriolis force and Lorentz force should be of comparable magnitude. Recent convective dynamo simulations reviewed here seem to resolve this caveat. We show that the available convective power indeed suffices to drive a magnetostrophic dynamo even when the heat flow though Mercury’s core–mantle boundary is subadiabatic, as suggested by thermal evolution models. Two possible causes are analyzed that could explain why the observations do not reflect a stronger internal field. First, toroidal magnetic fields can be strong but are confined to the conductive core, and second, the observations do not resolve potentially strong small-scale contributions. We review different dynamo simulations that promote either or both effects by (1) strongly driving convection, (2) assuming a particularly small inner core, or (3) assuming a very large inner core. These models still fall somewhat short of explaining the low amplitude of Mariner 10 observations, but the incorporation of an additional effect helps to reach this goal: The subadiabatic heat flow through Mercury’s core–mantle boundary may cause the outer part of the core to be stably stratified, which would largely exclude convective motions in this region. The magnetic field, which is small scale, strong, and very time dependent in the lower convective part of the core, must diffuse through the stagnant layer. Here, the electromagnetic skin effect filters out the more rapidly varying high-order contributions and mainly leaves behind the weaker and slower varying dipole and quadrupole components (Christensen in Nature 444:1056–1058, 2006). Messenger and BepiColombo data will allow us to discriminate between the various models in terms of the magnetic fields spatial structure, its degree of axisymmetry, and its secular variation.     

均匀磁场中铁磁流体润滑的轴颈轴承

当均匀外加磁场强度从0增加到 0.12 MA/m时, 在高剪切速率下铁磁流体润滑膜的承载能力提高25%,而在低剪切速率下, 承载能力可提高 35%。所以, 从实用的观点来看, 铁磁流体润滑是为了利用外磁场来调节轴承的承载性能, 而不是为了获得高承载力。为了避免轴承承载能力受到限制, 需要将铁磁流体密封与润滑膜分离开来。分析表明均匀磁场和剪切速率对姿态角的影响甚为微小。      

氧氮混合气体在梯度磁场中流动的数值模拟

用直接蒙特卡洛方法模拟了空气气流在梯度磁场中的氧浓度分布，利用DSMC模型将分子的碰撞和运动解耦，同时将磁场力简化为瞬间作用力，并对模拟结果进行了分析和对比。模拟表明，磁场强度与梯度乘积由100T^2／m增加到800T^2／m时，氧浓度由0．762％增加到3．1％；而当温度由0℃升高到100℃时，氧浓度由0．78％减小到0．25％。另外，随着压力的变化氧浓度存在一个最大值，在模拟条件下，这个最大值出现在0．05MPa(绝对压力)附近。