Where do flare ribbons stop?

The standard flare model,which was proposed based on observations and magnetohydrodynamic theory,can successfully explain many observational features of solar flares.However,this model is just a framework,with many details awaiting to be filled in, including how reconnection is triggered.In this paper,we address an unanswered question:where do flare ribbons stop?With the data analysis of the 2003 May 29 flare event,we tentatively confirmed our conjecture that flare ribbons finally stop at the intersection of separatrices(or quasi-separatrix layer in a general case)with the solar surface.Once verified,such a conjecture can be used to predict the final size and even the lifetime of solar flares.     

Filamentary structure on the Sun from the magnetic Rayleigh-Taylor instability

Magnetic flux emerges from the solar surface as dark filaments connecting small sunspots with opposite polarities. The regions around the dark filaments are often bright in X-rays and are associated with jets. This implies plasma heating and acceleration, which are important for coronal heating. Previous two-dimensional simulations of such regions showed that magnetic reconnection between the coronal magnetic field and the emerging flux produced X-ray jets and flares, but left unresolved the origin of filamentary structure and the intermittent nature of the heating. Here we report three-dimensional simulations of emerging flux showing that the filamentary structure arises spontaneously from the magnetic Rayleigh-Taylor instability, contrary to the previous view that the dark filaments are isolated bundles of magnetic field that rise from the photosphere carrying the dense gas. As a result of the magnetic Rayleigh-Taylor instability, thin current sheets are formed in the emerging flux, and magnetic reconnection occurs between emerging flux and the pre-existing coronal field in a spatially intermittent way. This explains naturally the intermittent nature of coronal heating and the patchy brightenings in solar flares.     

Continuous magnetic reconnection at Earth's magnetopause

The most important process that allows solar-wind plasma to cross the magnetopause and enter Earth's magnetosphere is the merging between solar-wind and terrestrial magnetic fields of opposite sense-magnetic reconnection. It is at present not known whether reconnection can happen in a continuous fashion or whether it is always intermittent. Solar flares and magnetospheric substorms--two phenomena believed to be initiated by reconnection--are highly burst-like occurrences, raising the possibility that the reconnection process is intrinsically intermittent, storing and releasing magnetic energy in an explosive and uncontrolled manner. Here we show that reconnection at Earth's high-latitude magnetopause is driven directly by the solar wind, and can be continuous and even quasi-steady over an extended period of time. The dayside proton auroral spot in the ionosphere--the remote signature of high-latitude magnetopause reconnection--is present continuously for many hours. We infer that reconnection is not intrinsically intermittent; its steadiness depends on the way that the process is driven.     

A current filamentation mechanism for breaking magnetic field lines during reconnection

During magnetic reconnection, the field lines must break and reconnect to release the energy that drives solar and stellar flares and other explosive events in space and in the laboratory. Exactly how this happens has been unclear, because dissipation is needed to break magnetic field lines and classical collisions are typically weak. Ion-electron drag arising from turbulence, dubbed 'anomalous resistivity', and thermal momentum transport are two mechanisms that have been widely invoked. Measurements of enhanced turbulence near reconnection sites in space and in the laboratory support the anomalous resistivity idea but there has been no demonstration from measurements that this turbulence produces the necessary enhanced drag. Here we report computer simulations that show that neither of the two previously favoured mechanisms controls how magnetic field lines reconnect in the plasmas of greatest interest, those in which the magnetic field dominates the energy budget. Rather, we find that when the current layers that form during magnetic reconnection become too intense, they disintegrate and spread into a complex web of filaments that causes the rate of reconnection to increase abruptly. This filamentary web can be explored in the laboratory or in space with satellites that can measure the resulting electromagnetic turbulence.     

Very fast optical flaring from a possible new Galactic magnetar

Highly luminous rapid flares are characteristic of processes around compact objects like white dwarfs, neutron stars and black holes. In the high-energy regime of X-rays and gamma-rays, outbursts with variabilities on timescales of seconds or less are routinely observed, for example in gamma-ray bursts or soft gamma-ray repeaters. At optical wavelengths, flaring activity on such timescales has not been observed, other than from the prompt phase of one exceptional gamma-ray burst. This is mostly due to the fact that outbursts with strong, fast flaring are usually discovered in the high-energy regime; most optical follow-up observations of such transients use instruments with integration times exceeding tens of seconds, which are therefore unable to resolve fast variability. Here we show the observation of extremely bright and rapid optical flaring in the Galactic transient SWIFT J195509.6+261406. Our optical light curves are phenomenologically similar to high-energy light curves of soft gamma-ray repeaters and anomalous X-ray pulsars, which are thought to be neutron stars with extremely high magnetic fields (magnetars). This suggests that similar processes are in operation, but with strong emission in the optical, unlike in the case of other known magnetars.     

DDS技术在高频电磁法仪器信号源中的应用

分析了锁相环技术与直接数字频率合成技术的工作原理，提出了结合两种技术设计高频电磁法仪器信号源的方法。克服了以往单纯采用锁相环技术设计信号源时跳频时间长、频率准确度低的弱点，测试结果显示，该方法设计的信号源频率准确度高，到小数点后两位，输出交、直流电压衰减小，达到信号源设计要求。     

Double Star TC-1 observation of the earthward flowing plasmoids in the near magnetotail

We analyze Double Star TC-1 magnetic field data from July to September in 2004 and find that plas-moids exist in the very near-Earth magnetotail. It is the first time that TC-1 observes the plasmoids inthe magnetotail at X > ?13 RE. According to the difference of the magnetic field structure in plasmoids,we choose two typical cases for our study: the magnetic flux rope on August 6 with the open magneticfield and the magnetic loop on September 14 with the closed magnetic field. Both of the cases are as-sociated with the high speed earthward flow and the magnetic loop is related to a strong substorm. Theions can escape from the magnetic flux rope along its open field line, but the case of the closed mag-netic loop can trap the ions. The earthward flowing plasmoids observed by TC-1 indicate that the mul-tiple X-line magnetic reconnection occurs beyond the distance of X=?10 RE from the earth.     

Electron dynamics in collisionless magnetic reconnection

Magnetic reconnection provides a physical mechanism for fast energy conversion from magnetic energy to plasma kinetic energy. It is closely associated with many explosive phenomena in space plasma, usually collisionless in character. For this reason, researchers have become more interested in collisionless magnetic reconnection. In this paper, the various roles of electron dynamics in collisionless magnetic reconnection are reviewed. First, at the ion inertial length scale, ions and electrons are decoupled. The resulting Hall effect determines the reconnection electric field. Moreover, electron motions determine the current system inside the reconnection plane and the electron density cavity along the separatrices. The current system in this plane produces an out-of-plane magnetic field. Second, at the electron inertial length scale, the anisotropy of electron pressure determines the magnitude of the reconnection electric field in this region. The production of energetic electrons, which is an important characteristic during magnetic reconnection, is accelerated by the reconnection electric field. In addition, the different topologies, temporal evolution and spatial distribution of the magnetic field affect the accelerating process of electrons and determine the final energy of the accelerated electrons. Third, we discuss results from simulations and spacecraft observations on the secondary magnetic islands produced due to secondary instabilities around the X point, and the associated energetic electrons. Furthermore, progress in laboratory plasma studies is also discussed in regard to electron dynamics during magnetic reconnection. Finally, some unresolved problems are presented.     

1999年8月16日EUV增亮事件数值研究的初步结果

我们基于TRACE卫星上EUV观测,采用三阶迎风紧致格式模拟了1999年8月16日EUV增亮事件。数值模拟结果可以给出这次EUV增亮事件的形成和演化过程的一种可能的解释。重联X点处最初的重联流可能与EUV增亮相对应。合并磁岛产生的高度叠加的抛射流,可能与最初表现为吸收特征随后表现为EUV发射结构的提升物质相对应。双向重联喷流可能与继续沿着似乎开放磁力线向上喷发,或流向太阳表面的提升物质相对应。     

Electron acceleration from contracting magnetic islands during reconnection

A long-standing problem in the study of space and astrophysical plasmas is to explain the production of energetic electrons as magnetic fields 'reconnect' and release energy. In the Earth's magnetosphere, electron energies reach hundreds of thousands of electron volts (refs 1-3), whereas the typical electron energies associated with large-scale reconnection-driven flows are just a few electron volts. Recent observations further suggest that these energetic particles are produced in the region where the magnetic field reconnects. In solar flares, upwards of 50 per cent of the energy released can appear as energetic electrons. Here we show that electrons gain kinetic energy by reflecting from the ends of the contracting 'magnetic islands' that form as reconnection proceeds. The mechanism is analogous to the increase of energy of a ball reflecting between two converging walls--the ball gains energy with each bounce. The repetitive interaction of electrons with many islands allows large numbers to be efficiently accelerated to high energy. The back pressure of the energetic electrons throttles reconnection so that the electron energy gain is a large fraction of the released magnetic energy. The resultant energy spectra of electrons take the form of power laws with spectral indices that match the magnetospheric observations.     

京津地区对流性和层状降水回波的特征分析

利用自动分类算法,识别出2005-2007年5-8月京津地区雷达回波中的对流性和层状降水回波.在此基础上,分析了该地区对流性和层状降水回波的垂直廓线和回波面积的日变化特征.结果表明:京津地区层状降水回波的垂直廓线在4 km高度(0℃)附近,出现了明显的"零度层亮带",亮带强度在当地夜间最强,当地上午最弱;该区域内,两种...     

广义非扩张集值映射的一个不动点定理

证明在Banach 空间中具有Opial 条件的弱紧凸集合上,多值平均非扩张自映射存在不动点,这一结论在单值情形下首次得到.     

基于四轴飞行器的双闭环PID控制

针对传统单闭环PID控制四轴飞行器存在的问题,设计并实现了一种双闭环PID控制算法。在姿态PID控制中,角度作为外环,角速度作为内环,运用姿态解算计算出欧拉角,作为姿态PID反馈量,进行姿态双闭环PID控制;在高度PID控制中,高度作为外环,z轴加速度作为内环,运用气压传感器采集的大气压值计算出高度,作为高度PID反馈量,进行高度双闭环PID控制。由于油门存在非线性问题,因此运用Matlab对油门转速曲线进行补偿,使输出的油门值近似线性化。飞行实验结果表明,四轴飞行器运用双闭环PID控制不仅反应快、超调量小,而且能够在室外稳定地飞行。     

J积分全塑性近似解及其在紧凑拉伸试样上的应用

将具有一定应变硬地指数的二维裂纹体在单一载荷作用处的位移分成线弹性部分和塑性部分。在平衡裂纹条件下，将塑性部分表达为该载荷与裂纹长度的函数。由此推得的Ｊ积分全塑性解析解具有适用于各种构形的一般性，且具有较高的精确度。本文将此解应用于紧凑拉伸试样，引用Ｃ．Ｆ，Ｓｈｉｈ等人的有限元结果及准解析解，发现本文得到的第二项比Ｍｅｒｋｌｅ－Ｃｏｒｔｅｎ公式的第二项具有明显优越的修正效能。     

Numerical study of magnetic reconnection process near interplanetary current sheet

The third order accurate upwind compact difference scheme has been applied to the numerical study of the magnetic reconnection process possibly occurring near the interplanetary current sheet, under the framework of the two-dimensional compressible magnetohydrodynamics (MHD). Our results here show that the driven reconnection near the current sheet can occur within 10—30 min for the interplanetary high magnetic Reynolds number, R_M =2 000—10 000, the stable magnetic reconnection structure can be formed in hour-order of magnitude, and there are some ba- sic properties such as the multiple X-line reconnections, vortical velocity structures, filament current systems, splitting and collapse of the high-density plasma bulk. These results are helpful in understanding and identifying the magnetic reconnection phenomena near the interplanetary current sheets.     

表面等离激元强弱耦合的频域和时域研究

从频域和时域两个维度研究表面等离激元耦合系统在强耦合与弱耦合区域的特性, 在理论上研究给定参数的表面等离激元耦合系统的本征频率、损耗以及亮暗模式随耦合强度的演化。在频域上对门结构在强耦合区域的杂化模式特征、散射光谱特性、偶极子与四极子模式的劈裂情况进行数值计算; 在时域上, 由于激发出两个不同频率的杂化模式叠加形成拍频, 利用拍频信号周期可以精确地给出杂化模式的频率, 得到散射光谱对应的频率不是精确的模式频率的结论。通过扫描耦合距离观察模式演化, 找到奇异点所处区域, 通过系统的频域响应拟合, 确定奇异点的位置。在弱耦合区域, 时域计算给出亮暗模式分别按自身衰减速率衰减的预期结果。     

Energetic electrons associated with magnetic reconnection in the sheath of interplanetary coronal mass ejection

Magnetic reconnection is an important universal plasma dissipation process that converts magnetic energy into plasma thermal and kinetic energy,and simultaneously changes the magnetic field topology.In this paper,we report the first observation of energetic electrons associated with asymmetric reconnection in the sheath of an interplanetary coronal mass ejection.The magnetic field shear angle was about 151°,implying guide-field reconnection.The width of the exhaust was about 8×104 km.The reconnection rate was estimated as 0.044-0.08,which is consistent with fast reconnection theory and previous observations.We observed flux enhancements of energetic electrons with energy up to 400 keV in this reconnection exhaust.The region where ener- getic electron fluxes were enhanced is located at one pair of separatrices in the higher density hemisphere.We discuss these observation results,and compare with previous observations and recent kinetic simulations.     

A magnetic reconnection X-line extending more than 390 Earth radii in the solar wind

Magnetic reconnection in a current sheet converts magnetic energy into particle energy, a process that is important in many laboratory, space and astrophysical contexts. It is not known at present whether reconnection is fundamentally a process that can occur over an extended region in space or whether it is patchy and unpredictable in nature. Frequent reports of small-scale flux ropes and flow channels associated with reconnection in the Earth's magnetosphere raise the possibility that reconnection is intrinsically patchy, with each reconnection X-line (the line along which oppositely directed magnetic field lines reconnect) extending at most a few Earth radii (R(E)), even though the associated current sheets span many tens or hundreds of R(E). Here we report three-spacecraft observations of accelerated flow associated with reconnection in a current sheet embedded in the solar wind flow, where the reconnection X-line extended at least 390R(E) (or 2.5 x 10(6) km). Observations of this and 27 similar events imply that reconnection is fundamentally a large-scale process. Patchy reconnection observed in the Earth's magnetosphere is therefore likely to be a geophysical effect associated with fluctuating boundary conditions, rather than a fundamental property of reconnection. Our observations also reveal, surprisingly, that reconnection can operate in a quasi-steady-state manner even when undriven by the external flow.     

交流变频软启动同步切换的实现

主要解决使用一台变频器带载软启动多台设备时所遇到的同步切换问题．借助锁相技术可使从变频器向工频电源切换的瞬间电压的大小频率和相位一致,达到平稳切换的目的．切换过程中电机电流不超过其额定电流的１．５倍,持续时间不超过数十ｍｓ     

太阳活动峰年和谷年期间黑子群与耀斑的统计分析

基于NOAA/SWPC公布的太阳活动数据,我们选取第24太阳活动峰年附近的12个连续月份(2011年7月至2012年6月)和第23太阳活动周谷年附近的12个连续月份(2005年7月至2006年6月),统计了这两段时间中太阳黑子群和耀斑的活动规律,并根据时间、黑子群分布纬度、寿命和磁场类型等对峰年和谷年进行了详细分析和比较,主要结论如下所述.(1)黑子群数随时间的变化在峰年和谷年均比较随机,峰年期间黑子数比谷年增多1.5倍左右.耀斑爆发与黑子群活动具有良好的相关性,但峰年期间存在某个月份耀斑数很少的现象,而谷年期间存在某个月份耀斑数集中增多的现象.(2)无论峰年还是谷年,δ类型黑子群的耀斑产率(耀斑总数与黑子群总数之比)最大,但β型黑子群产生的耀斑爆发最多.耀斑产率与磁场类型有密切关系,但与其所处太阳活动周中的阶段无关.(3)黑子群和耀斑的纬度分布的南北不对称性,以X级耀斑最为显著.峰年较谷年的耀斑数增加主要集中在C级和M级.(4)耀斑产率同黑子群寿命具有良好的相关性,但黑子群的数目同它们的寿命之间没有明显的规律.