Magnetic tornadoes as energy channels into the solar corona

Heating the outer layers of the magnetically quiet solar atmosphere to more than one million kelvin and accelerating the solar wind requires an energy flux of approximately 100 to 300?watts per square metre, but how this energy is transferred and dissipated there is a puzzle and several alternative solutions have been proposed. Braiding and twisting of magnetic field structures, which is caused by the convective flows at the solar surface, was suggested as an efficient mechanism for atmospheric heating. Convectively driven vortex flows that harbour magnetic fields are observed to be abundant in the photosphere (the visible surface of the Sun). Recently, corresponding swirling motions have been discovered in the chromosphere, the atmospheric layer sandwiched between the photosphere and the corona. Here we report the imprints of these chromospheric swirls in the transition region and low corona, and identify them as observational signatures of rapidly rotating magnetic structures. These ubiquitous structures, which resemble super-tornadoes under solar conditions, reach from the convection zone into the upper solar atmosphere and provide an alternative mechanism for channelling energy from the lower into the upper solar atmosphere.     

Observation and simulation of flux rope structures at the dayside magnetopause

The signatures of flux ropes with obvious core magnetic field are detected by Cluster Ⅱ at the dayside magnetopause during 11:00--11:15 UT on Mar. 2, 2001. The similar characteristics can be found from the magnetic fiel dvariations recorded by the four spacecrafts (Cluster Ⅱ C1--C4). All the three (-/ ) bipolar signatures in the BN component are accompanied with enhancements of BM and magnetic field strength B in the boundary normal coordinates (LMN coordinates). A MHD simulation with two dimensions and three components is performed to explore the reconnection process driven by the incoming flow of solar wind at the dayside magnetopause. The numerical results can illustrate the recurrent formation of magnetic structures with a core magnetic field. The time history of the magnetic field B and three components Bx, By and Bz at a given point of the current sheet can reproduce the observational features of the events mentioned above.     

太阳磁场的电流螺度、感应电场和能流分布研究

太阳光球磁场的动态演化在太阳爆发事件中起着重要作用。电流螺度、感应电场和坡印廷能流是表征磁场非势特性的典型参量。以活动区NOAA10488为例,利用局部相关跟踪方法,依据观测资料计算这3个参量,考察太阳光球磁场运动对于非势磁能的传输、释放作用。分析这个活动区的电流螺度、感应电场以及能流的分布,发现电流螺度和能流的分布情况均与太阳高层大气耀斑爆发密切相关,而感应电场的分布与其爆发的关系尚待进一步研究。     

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.     

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.     

电磁消涡与减震技术研究

利用流体边界层上的电磁体积力控制流体边界层的周期性脱落与分离,限制尾流涡街的产生,从而实现消除涡流和减少涡生震动的目的.理论分析和实验研究表明,当圆柱表面包覆的电磁场作用参数N＞1,包覆磁场强度B≥0.5 T,流体边界层表面电流密度j为103 A/m2数量级时,对于一般情况下的流场参数而言,流体边界层上的电磁体积力具有十分良好的消涡与减震控制作用效果.优化圆柱体表面的电磁场包覆范围,可以提高电磁消涡减震控制效率.当流体边界层上的电磁体积力方向与流体边界层的流动方向相反时,电磁力又具有显著的增涡增震控制作用效果.     

定量的太阳活动预报参数研究

Chumak[1987]提出来一个结构参数（文中称为有效距离参数）来定量地描述活动区磁场两极之间相互远离或者相互靠近的程度。这个参数将为定量研究活动区詹场位型演化研究，以及定量研究活动区磁场住型与太阳耀斑，日冕物质抛射等太阳活动的关系等开辟新的思路，Chumak，张洪起和郭娟对于这个参数的研究和应用做了一些研究工作，但是目前对这含参数的应用还不是很多。该文通过实际应用验缸有效距离参数探讨定量太阳活动预报参数的应用。我们将用有效距离参数，总磁通和磁倾角三个参数综合的定量的研究2011年2月15日一次X2.2级耀斑事件的演化情况。     

新型聚磁式横向磁场永磁推进同步电动机

针对现有的各种聚磁式横向磁场永磁电动机的定子结构较为复杂的问题,该文提出了一种新型聚磁式横向磁场永磁推进同步电动机结构。其主要特点是转子永磁体磁极采用三面墙式聚磁式结构,定子铁心由U形硅钢叠片构成,在提高了气隙磁密的同时简化了定子铁心的结构。利用三维电磁场有限元数值计算对该种电机的磁场进行了分析,并根据磁场分布计算了该种电机的电磁参数。实验结果与计算结果吻合较好。新型横向磁场永磁推进电机在保证电机性能的基础上简化了定子铁心结构。     

平行对极电磁铁磁场分布特性实验与研究

建立了平行对极电磁铁的三维模型,依据电磁效应原理,在齐次狄利克雷和诺依曼边界条件下,使用有限元法模拟仿真,得到了不同电流强度下,电磁铁对极间的三维磁感应强度分布特性,并用实验进行验证。结果表明:对极间磁感应强度在X和Z方向呈"V"型分布,在Y方向呈倒"V"形分布,模拟仿真与实测结果变化趋势基本一致;在同一参数下,测量基准面左右两侧的磁感应强度值是中心区域的2~5倍,电磁铁内侧的磁感应强度值大于外侧,且与基准面距离的平方成反比;磁感应强度均值在水平方向与位移的平方成正比。     

湍流边界层雷诺应力和壁脉动压强相位滞后分析

在风洞平板湍流边界层外层引入圆柱尾涡的周期性扰动,在尾流干扰下的湍流边界层内进行测量,对相位滞后关系进行了实验研究,给出了湍流边界层内的雷诺应力和壁面脉动压强相对于边界层内的大尺度结构变形率的相位滞后沿壁面法向的变化趋势,分析结果表明剪切湍流涡粘模式中的涡粘系数应该是随时均流梯度变化的复数形式.     

从不稳定到近中性大气边界层的大涡模拟

用大涡模拟方法对不稳定到近中性层结的大气边界层情况进行模拟。模拟条件为：地面运动学热通量0.0001～0.2 K·m·s^-1、地转驱动风速0～15 m·s^-1,对应的无因次稳定度参数 - z/L 为0.0062～368。模拟结果显示,大气边界层直到 - z/L＝0.668的近中性情况,其热通量和动量通量等仍保留着典型对流边界层的基本特征,可由模式较好地求解,且在近地面与观测结果相符较好。对更接近中性的情况,模式分辨率限制了对边界层湍流特性的求解。在大风、弱不稳定边界层条件下模拟发现有滚动涡现象出现,其稳定度范围大致对应- z/L 的取值0.668～24.6。     

Three-dimensional magnetic field topology in a region of solar coronal heating

Flares and X-ray jets on the Sun arise in active regions where magnetic flux emerges from the solar interior amd interacts with the ambient magnetic field. The interactions are believed to occur in electric current sheets separating regions of opposite magnetic polarity. The current sheets located in the corona or upper chromosphere have long been thought to act as an important source of coronal heating, requiring their location in the corona or upper chromosphere. The dynamics and energetics of these sheets are governed by a complex magnetic field structure that, until now, has been difficult to measure. Here we report the determination of the full magnetic vector in an interaction region near the base of the solar corona. The observations reveal two magnetic features that characterize young active regions on the Sun: a set of rising magnetic loops and a tangential discontinuity of the magnetic field direction, the latter being the observational signature of an electric current sheet. This provides strong support for coronal heating models based on the dissipation of magnetic energy at current sheets.     

地磁活动指数与太阳活动的小波分析

根据1957—2012年的地磁指数Ap、Dst、AE和太阳活动参数(太阳黑子相对数R与太阳射电流量F10.7)数据,利用小波分析方法研究了地磁活动与太阳活动的关系.结果表明,Ap、Dst、AE指数和太阳活动参数均存在准11 a和准22 a的周期特征.Ap和AE峰值滞后于太阳参数峰值1~2 a;而Dst指数与太阳参数存在近似负相关的关系,但从第21太阳周起逐渐延迟于太阳参数,表明地磁活动受太阳活动影响的滞后性.此外,地磁指数峰值从第20太阳周开始有逐渐下降的趋势,反映了地磁活动对太阳活动的响应减弱.     

冕洞边界区磁结构的探讨

摘要用Hell083nm单色像上的极区、低纬冕洞的边界,确定Fe]532.4nm纵向场全日面磁图上对应的极,低纬冕洞的边界.对光球上极、低纬冕洞边界足根连线范围内外的磁场强度,磁极性、磁场几何位形进行了分析讨论.观测结果表明t就极无涧大尺度范围来看,是单极开放场I就48h时标的加强磁结构来说,以开放场为主的情况下,有开放场与闭合场栩混杂的情况.就同时的极冕洞与低纬度冕洞边界足根连线附近磁场位形相比较,差别是明显的.     

Thermochemical flows couple the Earth's inner core growth to mantle heterogeneity

Seismic waves sampling the top 100 km of the Earth's inner core reveal that the eastern hemisphere (40 degrees E-180 degrees E) is seismically faster, more isotropic and more attenuating than the western hemisphere. The origin of this hemispherical dichotomy is a challenging problem for our understanding of the Earth as a system of dynamically coupled layers. Previously, laboratory experiments have established that thermal control from the lower mantle can drastically affect fluid flow in the outer core, which in turn can induce textural heterogeneity on the inner core solidification front. The resulting texture should be consistent with other expected manifestations of thermal mantle control on the geodynamo, specifically magnetic flux concentrations in the time-average palaeomagnetic field over the past 5 Myr, and preferred eddy locations in flows imaged below the core-mantle boundary by the analysis of historical geomagnetic secular variation. Here we show that a single model of thermochemical convection and dynamo action can account for all these effects by producing a large-scale, long-term outer core flow that couples the heterogeneity of the inner core with that of the lower mantle. The main feature of this thermochemical 'wind' is a cyclonic circulation below Asia, which concentrates magnetic field on the core-mantle boundary at the observed location and locally agrees with core flow images. This wind also causes anomalously high rates of light element release in the eastern hemisphere of the inner core boundary, suggesting that lateral seismic anomalies at the top of the inner core result from mantle-induced variations in its freezing rate.     

Solar chromospheric spicules from the leakage of photospheric oscillations and flows

Spicules are dynamic jets propelled upwards (at speeds of approximately 20 km s(-1)) from the solar 'surface' (photosphere) into the magnetized low atmosphere of the Sun. They carry a mass flux of 100 times that of the solar wind into the low solar corona. With diameters close to observational limits (< 500 km), spicules have been largely unexplained since their discovery in 1877: none of the existing models can account simultaneously for their ubiquity, evolution, energetics and recently discovered periodicity. Here we report a synthesis of modelling and high-spatial-resolution observations in which numerical simulations driven by observed photospheric velocities directly reproduce the observed occurrence and properties of individual spicules. Photospheric velocities are dominated by convective granulation (which has been considered before for spicule formation) and by p-modes (which are solar global resonant acoustic oscillations visible in the photosphere as quasi-sinusoidal velocity and intensity pulsations). We show that the previously ignored p-modes are crucial: on inclined magnetic flux tubes, the p-modes leak sufficient energy from the global resonant cavity into the chromosphere to power shocks that drive upward flows and form spicules.     

The unusual minimum of sunspot cycle 23 caused by meridional plasma flow variations

Direct observations over the past four centuries show that the number of sunspots observed on the Sun's surface varies periodically, going through successive maxima and minima. Following sunspot cycle 23, the Sun went into a prolonged minimum characterized by a very weak polar magnetic field and an unusually large number of days without sunspots. Sunspots are strongly magnetized regions generated by a dynamo mechanism that recreates the solar polar field mediated through plasma flows. Here we report results from kinematic dynamo simulations which demonstrate that a fast meridional flow in the first half of a cycle, followed by a slower flow in the second half, reproduces both characteristics of the minimum of sunspot cycle 23. Our model predicts that, in general, very deep minima are associated with weak polar fields. Sunspots govern the solar radiative energy and radio flux, and, in conjunction with the polar field, modulate the solar wind, the heliospheric open flux and, consequently, the cosmic ray flux at Earth.     

基于支持向量机和k近邻的太阳质子事件预报模型

应用支持向量机和k近邻相结合的方法,建立了太阳质子事件预报模型。预报因子包括黑子面积、磁分型、McIntosh分型、太阳射电流量、活动区位置和软X射线流量。太阳质子事件模型包括两个子模型：质子有无模型和质子峰值流量模型。质子有无模型能对未来24小时是否发生质子事件给出预报,质子峰值流量模型对已发生的质子事件预报峰值流量等级。用2002年和2004年的数据进行了模拟预报,结果显示模型具有较高的报准率,同时显示出活动区位置和软x射线通量是比较敏感的预报因子。     

Mesoscopic superconductor as a ballistic quantum switch.

Several key experiments have revealed a rich variety of vortex structures in mesoscopic superconductors in which only a few quanta of magnetic flux are trapped: these structures are polygon-like vortex 'molecules' and multi-quanta giant vortices. Ginzburg-Landau calculations confirmed second-order phase transitions between the giant vortex states and stable molecule-like configurations. Here we study theoretically the electronic structure and the related phase-coherent transport properties of such mesoscopic superconductor systems. The quasiparticle excitations in the vortices form coherent quantum-mechanical states that offer the possibility of controlling the phase-coherent transport through the sample by changing the number of trapped flux quanta and their configuration. The sample conductance measured in the direction of the applied magnetic field is determined by the transparency of multi-vortex configurations, which form a set of quantum channels. The transmission coefficient for each channel is controlled by multiple Andreev reflections within the vortex cores and at the sample edge. These interference phenomena result in a stepwise behaviour of the conductance as a function of the applied magnetic field, and we propose to exploit this effect to realize a vortex-based quantum switch where the magnetic field plays the role of the gate voltage.     

Ignition of global wildfires at the Cretaceous/Tertiary boundary

An impressive amount of evidence supports the proposal of Alvarez et al. that the Cretaceous era was ended abruptly by the impact of a comet or asteroid. The recent discovery of an apparently global soot layer at the Cretaceous/Tertiary boundary indicates that global wildfires were somehow ignited by the impact. Here we show that the thermal radiation produced by the ballistic re-entry of ejecta condensed from the vapour plume of the impact could have increased the global radiation flux by factors of 50 to 150 times the solar input for periods ranging from one to several hours. This great increase in thermal radiation may have been responsible for the ignition of global wildfires, as well as having deleterious effects on unprotected animal life.