角区三维漩涡流动的新分离结构

分别用数值计算和PIV(Particle Image Velocimetry)实验方法研究角区层流边界层三维定常分离的流动结构,证实了角区确实存在有别于传统分离现象的附着鞍点结构,对称面上游的流线并非从壁面向上抬起从壁面分离,而是经由空间某个奇点向壁面附着.角区马蹄涡的传统分离鞍点结构和附着鞍点结构之间存在着一定的演化规律,影响参数包括模型头部钝度、边界层厚度和雷诺数.一定的边界层和雷诺数条件下随着模型头部钝度减小,角区马蹄涡将从传统的分离鞍点结构逐步过渡为附着鞍点结构;对一定的模型若雷诺数越大、边界层越厚则角区流动越趋向于传统的分离鞍点结构,反之则倾向于附着鞍点结构.     

角区三维分离流附着鞍点拓扑结构及其演化

实验研究角区层流边界层三维定常分离附着鞍点拓扑结构的存在性及其演化规律.二维粒子图像测速(PIV,Particle Image Velocimetry)激光片光源设置于给定平板和不同模型组成的角区对称面,采用微距镜头捕捉对称面奇点附近的局部流动拓扑结构.实验证实在一定流动参数条件下多种形状模型与平板形成的角区均存在有别于经典分离的附着鞍点拓扑结构;随着雷诺数增加或者随着模型钝度的变化,附着鞍点拓扑结构与经典分离鞍点拓扑结构之间存在着一定的演化规律;对附着鞍点拓扑结构与Lighthill经典三维分离模式的关系进行了分析,表明Lighthill经典三维分离模式也适用于分析附着鞍点拓扑结构.     

极端太阳风条件下的磁层顶位形

基于极端太阳风条件下的三维MHD数值模拟数据, 构建了一种极端太阳风条件下的三维非对称磁层顶位形模型. 所提出的模型考虑了行星际南向磁场(IMF) B_z日下点距离侵蚀的饱和效应, 太阳风动压B_d对磁层顶张角影响的饱和效应, 赤道面、昼夜子午面磁层顶的不对称性以及极尖区的内凹结构和内凹中心的移动, 并利用Levenberg-Marquart多参量非线性拟合方法拟合了模型参数. 数值模拟研究表明, 在极端太阳风条件下, 随B_d增大, 磁层顶日下点距离减小, 磁层顶磁尾张角几乎不变; 随南向(IMF)B_z增大, 磁层顶日下点距离略有减小, 磁层顶磁尾张角减小, 极尖区内凹中心向低纬移动. 通过对2010年8月1日太阳风暴事件验证发现, 本文所建立的模型能够描述极端太阳风条件下的三维磁层顶位形.      

极小化相位误差加权间断有限元辛方法

对于线性Hamilton系统,辛差分方法可以保持系统的辛结构,有限元方法可以保证系统的辛性质并具有能量守恒特性。但辛差分方法和有限元方法时域上仍然存在相位误差,使得计算的精度不是很理想。提出极小化相位误差加权间断有限元辛方法（WDG-PF）,该方法是辛方法,同时,对Hamilton系统的求解具有极小的相位误差。数值显示该方法可以保证Hamilton系统的能量守恒性。WDG-PF方法解决了时间有限元方法（TFE）存在的相位漂移现象,同时指出间断有限元方法可以通过加权处理达到保辛要求。WDG-PF方法相较于针对相位误差设计的计算格式分数步对称辛算法（FSJS）、辛Runge-Kutta-Nystrom（RKN）格式以及辛分块Runge-Kutta（SPRK）等方法,WDG-PF显著地减少相位误差,和显著提高Hamilton系统能量精度的优点。相位误差和能量误差几乎达到计算机精度。同时单元内部具有超收敛现象。特别针对高低混频Hamilton系统,传统方法很难在固定的步长下同时实现对高频和低频信号的精确仿真,WDG-PF方法则可以在大步长下同时实现对低频信号和高频信号的高精度仿真。数值显示,WDG-PF方法切实有效。      

HF wave activity in the low and middle-altitude polar cusp

We reported the results of our investigations of wave activity in high-frequency range performed on board CLUSTER spacecraft in the middle-altitude cusp region, around 5 R_E during August and September 2002. Our analysis was mainly based on the registration gathered by the WHISPER instrument (Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation). For a better understanding of the processes of wave-particle interaction and in order to understand the general plasma conditions in the cusp region, we also included in our analysis the data registered by the STAFF (Spatio-Temporal Analysis of Field Fluctuation experiment) instrument and the CIS (Ion Spectrometry experiment) instrument. These observations were carried out during different geomagnetic activity; under quiet conditions and during magnetic storm period. The space plasma is characterised by the ratio of plasma frequency to electron gyrofrequency, in this case, the local plasma frequency was, mainly, a little greater than the electron plasma, but it was also frequently observed that these two characteristic frequencies were not very different from one another. The whistler waves, electron-cyclotron waves, electron-acoustic waves and Langmuir waves have been detected when the spacecraft was crossing the middle-altitude cusp region. We suggested that the majority of those waves were generated by electron beams. For a better understanding the plasma conditions in the low and middle-altitude cusp region the past FREJA wave data results are used to describe typical wave activity detected in the low-altitude cusp region. The aim of this paper is to discuss, on the basis of a few chosen representative examples, the property of typical high wave activity detected in the lower part of cusp region.     

树形多体Hamilton系统的Lyapunov指数计算方法

研究了树形多体Hamilton系统Lyapunov指数的数值方法.利用多体Hamilton系统的正则方程和辛算法, 给出了多体Hamilton系统Lyapunov指数的计算方法,该算法具有较好的计算精度和通用性.利用该算法可对系统的运动稳定性进行分析.最后用算例说明了该算法的有效性.      

有界双重控制导弹微分对策制导律

针对有界控制导弹采用鸭舵或尾舵单一控制形式存在的劣势,基于双边优化微分对策理论,推导了一种有界双重控制导弹微分对策制导律。该制导律不仅将鸭舵与尾舵两组舵面的控制有效融合在一起,而且实现了有界控制命令最优的分配设计。分析了该微分对策制导律的对策空间,并从弹目机动性能比和控制系统时间常数比之间的关系,给出了鞍点解的存在条件。考虑非完全信息情形,完成了目标加速度滤波器和拦截性能衡量指标的设计。采用Monte Carlo法进行了制导性能的仿真验证,结果表明:所设计的有界双重控制导弹制导律与采用单一的鸭舵控制或尾舵控制的导弹相比不仅机动性要求较低,且具有较高的命中概率。      

Multiple Sun–Earth Saddle Point flybys for LISA Pathfinder

LISA Pathfinder is an ESA mission due to be launched in the next two years. The gravity gradiometer onboard has the sensitivity required to test predictions by gravitational theories proposed as alternatives to Dark Matter such as TeVeS. Within the Solar System measurable effects are predicted only in the vicinity of gravitational saddle points (SP). For this reason it has been proposed to fly LPF by the Earth–Sun SP, at some 259,000 km from Earth. This could be done in an extension to the nominal mission which uses a Lissajous orbit about the Earth–Sun L1 point. The responsibility for LPF mission design lies with ESA/ESOC, who have designed the transfer trajectories, orbits about L1, and station keeping strategies. This article describes an analysis performed by Astrium to support a suggestion for a possible mission extension to a saddle point crossing. With only very limited fuel availability, reaching the saddle point is a significant challenge. In this article, we present recent advances in the work on trajectory design. It is demonstrated that reaching the SP is feasible once the LPF mission is completed. Furthermore, in a significant enhancement, it is demonstrated that trajectories including more than one SP flyby are possible, thus improving the science return for this proposed mission extension.     

Plasma flow across the cusp-magnetosheath boundary under northward IMF

In this paper, we have used two closely spaced (INTERBALL-1 and MAGION-4) satellites orbiting in the region adjacent to the magnetopause with motivation to determine the structure of the cusp-magnetosheath boundary under steady solar wind conditions and under the northward interplanetary magnetic field (IMF). Two-point observations reveal that a steady reconnection takes place tailward of the cusp and the position of the reconnection site moves in accordance with the actual IMF direction. Reconnection produces a latitudinally dispersed cusp precipitation with highest energies in the cusp poleward edge. The reconnection site is widely spread in local time and thus changes of the IMF By component only slightly modulate observed patterns. The change of the plasma flow direction suggests the presence of the vortex-like structure in the exterior cusp.     

Improving the angular resolution of EGRET and new limits on supersymmetric dark matter near the galactic center

Using the EGRET data and an improved point source analysis, including an energy-dependent point spread function and an unbinned maximum likelihood technique, we have been able to place considerably lower limits on the γ-ray flux from the galactic center region. We also test this method on known sources, the Crab and Vela pulsars. In both cases, we find that our method improves the angular precision of EGRET data over the 3EG catalog.This new limit on γ-rays from the galactic center can be used to test models of annihilating supersymmetric dark matter and galactic halo profiles. We find that the present EGRET data can limit many supersymmetric models if the density of the galactic dark matter halo is cuspy or spiked toward the galactic center. We also discuss the ability of GLAST to test these models.     

等离子体密度对栅极系统束流影响分析

针对现有离子推力器栅极系统束流引出分析中未考虑放电室等离子体密度均匀性影响的不足,基于数值方法对该问题进行了研究。采用单元内粒子 （Particle In Cell,PIC） 方法对栅极系统束流引出进行了数值模拟。PIC方法中电场求解采用有限差分方法,离子加速方法采用跳蛙格式。以国产20cm Xe离子推力器作为算例,计算得到了栅极中心和边缘孔引出束流离子和电场的分布。结果显示栅极中心孔相对边缘孔束流聚焦性好,束流发散角小,但中心孔轴线的鞍点电势较边缘孔高24.8V。因此,放电室等离子体密度分布对束流引出具有重要影响,电子返流现象最先出现在栅极中心位置。     

Two sources of magnetosheath ions observed by Cluster in the mid-altitude polar cusp

Double cusps have been observed on a few occasions by polar orbiting spacecraft and ground-based observatories. The four Cluster spacecraft observed two distinct regions, showing characteristics of a double cusp, during a mid-altitude cusp pass on 7 August 2004. The Wind spacecraft detected a southward turning of the Interplanetary Magnetic Field (IMF) at the beginning of the cusp crossings and IMF–Bz stayed negative throughout. Cluster 4 observed a high energy step in the ion precipitation around 1 keV on the equatorward side of the cusp and a dense ion population in the cusp centre. Cluster 1, entering the cusp around 1 min later, observed only a partial ion dispersion with a low energy cutoff reaching 100 eV, together with the dense ion population in the cusp centre. About 9 min later, Cluster 3 entered the cusp and observed full ion dispersion from a few keV down to around 50 eV, together with the dense ion population in the centre of the cusp. The ion flow was directed poleward and eastward in the step/dispersion, whereas in the centre of the cusp the flow was directed poleward and westward. In addition the altitude of the source region of ion injection in the step/dispersion was found 50% larger than in the cusp centre. This event could be explained by the onset of dayside reconnection when the IMF turned southward. The step would be the first signature of component reconnection near the subsolar point, and the injection in the centre of the cusp a result of anti-parallel reconnection in the northern dusk side of the cusp. A three-dimensional magnetohydrodynamic (MHD) simulation is used to display the topology of the magnetic field and locate the sources of the ions during the event.     

陀螺仪运动的复杂性

建立了外环轴水平放置的重力对称陀螺仪的运动方程.并将陀螺仪转子的质心位置作为扰动, 在一定条件下, 首先研究了自由陀螺仪的运动, 并给出力学意义解释; 然后利用Melnikov方法和KAM理论研究了非自由陀螺仪的运动.研究结果表明: 在陀螺仪转子的质心与支架中心不重合且充分接近, 或陀螺仪能量充分大时, 陀螺仪的运动出现Smale马蹄意义下的混沌; 同时它的Hamiltonian流存在KAM不变环面和不变闭曲线.      

基于数据中台的数据融合集成关键技术研究

当前开发新的业务系统往往需要从其他系统引接数据,系统之间的直接数据交互增加了系统开发的复杂性。为解决上述问题,研究基于数据中台的数据融合集成关键技术,为数据中台建设提供参考。设计数据中台技术架构,实现数据引接、数据管理和数据服务。覆盖数据生命周期,设计数据中台业务流程。瞄准数据赋能目标,提升数据融合集成核心能力,采用混合架构完成多源异构数据存储,利用数据层次模型实现数据映射,应用知识图谱进行数据关联。本文提出的数据中台技术架构已在实际项目中运用,达到预期效果。     

Testing Modified Newtonian Dynamics with LISA Pathfinder

We suggest that LISA Pathfinder, a technology demonstrator for the future gravitational wave observatory LISA, could be used to carry out a direct experimental test of Modified Newtonian Dynamics (MOND). The LISA Pathfinder spacecraft is currently being built and the launch date is just a few years away. No modifications of the spacecraft are required, nor any interference with its nominal mission. The basic concept is to fly LISA Pathfinder through the region around the Sun-Earth saddle point, in an extended mission phase, once the original mission goals are achieved. We examine various strategies to reach the saddle point, and find that the preferred strategy, yielding relatively short transfer times of just over 1 year, probably involves a lunar fly-by. LISA Pathfinder will be able to probe the intermediate MOND regime, i.e. the transition between deep MOND and Newtonian gravity. We present robust estimates of the anomalous gravity gradients that LISA Pathfinder should be exposed to, based on MONDian effects as derived from the Tensor-Vector-Scalar (TeVeS) theory. The spacecraft speed and spatial scale of the MOND signal combine in a way that the spectral signature of the signal falls precisely into LISA Pathfinder’s measurement bandwidth. We find that if the gravity gradiometer on-board the spacecraft achieves its currently predicted sensitivity, these anomalous gradients could not just be detected, but measured in some detail.     

Magnetic field disturbances in the mid-altitude cusp

Magnetic field disturbances and hot particles in the cusp as seen mainly by both the IMAP-3 magnetometer and PROMICS -3 spectrometer aboard the INTERBALL-AURORAL PROBE (AU) (perigee 4 Re, inclination 65 deg) are discussed. Orbits from March, 1997 are analysed accordingly. The INTERBALL-AU transits cross the middle of the cusp from low to high latitude from pre-noon to post-noon hours 11–13 MLT. Although the crossings are not exactly meridional, they reach 80–81 ILAT and permitting detection of the cusp, its subregions and their equatorward and poleward boundaries. Magnetic field disturbances are analysed for field-aligned currents (FACs) during different IMF conditions. Regions with structured forms are emphasised, in particular where a more intense current is concentrated. The following cases are compared: (a) the most intense current in the boundary cusp, adjacent to the ring current (March 7, southward IMF); (b) FACs are concentrated completely inside the cusp (March 13, southward -downward IMF) and (c) FACs with pronounced intensities equatorward from the cusp proper (March 11, duskward IMF).     

Influence of Earth’s shadowing effects on space debris stability

Solar radiation pressure affects the evolution of high area-to-mass geostationary space debris. In this work, we extend the stability study of Valk et al. (2009) by considering the influence of Earth’s shadows on the short- and long-term time evolutions of space debris. To assess the orbits stability, we use the Mean Exponential Growth factor of Nearby Orbits (MEGNO), which is an efficient numerical tool to distinguish between regular and chaotic behaviors. To reliably compute long-term space debris motion, we resort to the Global Symplectic Integrator (GSI) of Libert et al. (2011) which consists in the symplectic integration of both Hamiltonian equations of motion and variational equations. We show how to efficiently compute the MEGNO indicator in a complete symplectic framework, and we also discuss the choice of a symplectic integrator, since propagators adapted to the structure of the Hamiltonian equations of motion are not necessarily suited for the associated variational equations. The performances of our method are illustrated and validated through the study of the Arnold diffusion problem. We then analyze the effects of Earth’s shadows, using the adapted conical and cylindrical Earth’s shadowing models introduced by Hubaux et al. (2012) as the smooth shadow function deriving from these models can be easily included into the variational equations. Our stability study shows that Earth’s shadows greatly affect the global behaviour of space debris orbits by increasing the size of chaotic regions around the geostationary altitude. We also emphasize the differences in the results given by conical or cylindrical Earth’s shadowing models. Finally, such results are compared with a non-symplectic integration scheme.     

A question raised from the observation of dynamic cusp formation: When and where does particle acceleration occur?

We present observations of a C9.4 flare on 2002 June 2 in EUV (TRACE) and X-rays (RHESSI). The multiwavelength data reveal: (1) the involvement of a quadrupole magnetic configuration; (2) loop expansion and ribbon motion in the pre-impulsive phase; (3) gradual formation of a new compact loop with a long cusp at the top during the impulsive phase of the flare; (4) appearance of a large, twisted loop above the cusp expanding outward immediately after the hard X-ray peak; and (5) X-ray emission observed only from the new compact loop and the cusp. In particular, the gradual formation of an EUV cusp feature is very clear. The observations also reveal the timing of the cusp formation and particle acceleration: most of the impulsive hard X-rays (>25 keV) were emitted before the cusp was seen. This suggests that fast reconnection occurred during the restructuring of the magnetic configuration, resulting in more efficient particle acceleration, while the reconnection slowed after the cusp was completely formed and the magnetic geometry was stabilized. This observation is consistent with the observations obtained with Yohkoh/Soft X-ray Telescope (SXT) that soft X-ray cusp structures only appear after the major impulsive energy release in solar flares. These observations have important implications for the modeling of magnetic reconnection and particle acceleration.     

磁层顶极尖区的理论探讨

本文解出了三维磁层顶的Chapman-Ferraro模型。证明极尖区有一条极尖线,长约40°。磁尖线上磁层顶呈尖角。磁层磁力线由极尖线上各点通往磁层顶。通常所谓中性点,足极尖线在日地子午面的截点。