Particle Acceleration and Nonthermal Phenomena in Superbubbles

Models of nonthermal particle acceleration in the vicinity of active star forming regions are reviewed. We discuss a collective effect of both stellar winds of massive stars and core collapsed supernovae as particle acceleration agents. Collective supernova explosions with great energy release in the form of multiple interacting shock waves inside the superbubbles are argued as a favourable site of nonthermal particle acceleration. The acceleration mechanism provides efficient creation of a nonthermal nuclei population with a hard low-energy spectrum, containing a substantial part of the kinetic energy released by the winds of young massive stars and supernovae. We discuss a model of temporal evolution of particle distribution function accounting for the nonlinear effect of the reaction of the accelerated particles on the shock turbulence inside the superbubble. The model illustrates that both the low-energy metal-rich nonthermal component and the standard galactic cosmic rays could be efficiently produced by superbubbles at different evolution stages.     

轴流压气机转子尖部三维复杂流动Ⅰ——实验和理论研究

在低速大尺寸压气机实验台上,利用体视图像粒子测速(SPIV)技术测量了设计状态和近失速状态转子尖部的三维复杂流动,对典型二次流流动结构的特性及其产生、发展和演化机制做了研究。实验测量覆盖整个转子通道,从测量得到的各阶物理量中可以识别出叶尖泄漏涡、角区旋涡、通道涡和进口导叶尾迹等多种二次流流动结构。通过分析各种二次流流动结构造成的流动堵塞和损失发现:在设计状态,叶尖泄漏涡是流动堵塞和损失的主要来源,在转子出口处造成的流动堵塞约为总流量的0.35%;在近失速状态,角区旋涡对流动堵塞和损失的分布起了决定性作用,造成的流动堵塞可以达到总流量的8.5%。最后,借鉴二次流理论对角区旋涡的产生、发展和演化机制做了理论分析,结果表明角区旋涡的发展过程主要由流向速度的展向分布规律决定。     

The Pre-CME Sun

The coronal mass ejection (CME) phenomenon occurs in closed magnetic field regions on the Sun such as active regions, filament regions, transequatorial interconnection regions, and complexes involving a combination of these. This chapter describes the current knowledge on these closed field structures and how they lead to CMEs. After describing the specific magnetic structures observed in the CME source region, we compare the substructures of CMEs to what is observed before eruption. Evolution of the closed magnetic structures in response to various photospheric motions over different time scales (convection, differential rotation, meridional circulation) somehow leads to the eruption. We describe this pre-eruption evolution and attempt to link them to the observed features of CMEs. Small-scale energetic signatures in the form of electron acceleration (signified by nonthermal radio bursts at metric wavelengths) and plasma heating (observed as compact soft X-ray brightening) may be indicative of impending CMEs. We survey these pre-eruptive energy releases using observations taken before and during the eruption of several CMEs. Finally, we discuss how the observations can be converted into useful inputs to numerical models that can describe the CME initiation.     

PARAMETER IDENTIFICATION METHOD OF NONLINEAR JOINTS

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基于非线性渐进损伤模型的复合材料波纹梁耐撞性能研究

基于连续介质损伤力学,提出了一种包括层内和层间失效的非线性渐进损伤模型来预测复合材料波纹梁在轴向冲击下的失效行为。其中,层内损伤采用最大应力准则,并结合指数型损伤演化法则和刚度折减方法预测失效后的材料参数。层间损伤模型则采用了二次名义应力准则、基于混合模式能量的指数型损伤演化法则和黏性刚度折减方法建立。基于该模型,对典型的波纹梁结构参数和触发等对耐撞性的影响进行了研究。结果表明数值模拟结果与试验结果基本吻合,模型能够准确地模拟复合材料波纹梁在冲击过程中出现的分层、纤维和基体破坏等失效模式。波纹梁在破坏过程中吸收的能量、比吸能和载荷峰值随层数不断递增,降低高度和减小触发结构的截面面积均会降低载荷峰值。     

Nonlinear modal electromechanical coupling factor for piezoelectric structures containing nonlinearities

Within the linear framework, the Modal Electromechanical Coupling Factor (MEMCF) is an important indicator to quantify the dynamic conversion of mechanical energy and electrical energy of piezoelectric structures. It is also an important tool to guide the piezoelectric damping design of linear structures. Advanced aircraft often fly in maneuvers, and the variable working conditions induce drastic changes in the load level on structures. Geometric and contact nonlinearities of thin-walled structures and joint structures are often activated. To achieve a good vibration reduction effect covering all working conditions, one cannot directly use linear electromechanical coupling theory to instruct the piezoelectric damping design for nonlinear structures. Therefore, this paper defines the Nonlinear Modal Electromechanical Coupling Factor (NMEMCF) and proposes the corresponding numerical method for the first time to quantitatively evaluate the electromechanical coupling capability of nonlinear piezoelectric structures. Three candidate definitions of the NMEMCF are given, including two frequency definitions and one energy definition. The energy definition is the most promising one. It is not only applicable to both conservative and dissipative nonlinear structures but also compatible with the linear MEMCF. In addition, based on the energy formula, the NMEMCF can be obtained by only performing one nonlinear modal analysis in the open-circuit state. The analytical findings and the numerical tool are validated against two piezoelectric structures with different types of nonlinearities. A strong correlation among the NMEMCF, geometric parameters, and energy dissipation is observed. The results confirm that the proposed NMEMCF captures the physics of the electromechanical coupling phenomenon associated with nonlinear piezoelectric structures and can be used as an essential design indicator of piezoelectric damping, especially for variable working conditions.     

Detailed magnetic structure and stochastic threshold

Non-linear evolution of reconnection is too slow to explain-by itself-fast phenomena such as internal disruptions in tokamaks or flares in the solar atmosphere. It has been proposed that the change in topology could lead to field line stochastization, and hence to highly increased transport. An important objection to this idea is that the increase of transport coefficients should smoothly follow the amplitude of the perturbation, while the observations show a catastrophic transition. We have shown 1) that the shape of the structures (and not only their size or amplitude) evolve during non-linear evolution 2) that the stochastic threshold can be strongly influenced by the detailed shape. Therefore, sharp transitions can appear during the evolution, due to the combination of these two effects. We will first consider an idealized situation, namely the two-waves problem in slab geometry, for which we will study the effect of the separatrix shape on the stochastic threshold. In the second part, we will present an application to the internal disruption in tokamaks, with anm=1 perturbation in a toroidal magnetic configuration. In the last part, we will discuss possible applications of the studies on shape effects to the behaviour of trapped particles in structures of the solar atmosphere.     

Smart card information and operations using biometrics

Nowadays many systems need a portable media to store some sensible data, such as smart cards. The information can be protected by the user with his Personal Identification Number (PIN), or through biometrics. Unfortunately, there is not a smart card today that can verify the biometric template inside it, performing this task in the terminal. The author has developed the algorithms and data structures needed to solve this problem. Therefore, he has created a smart card with user biometric authentication, based on an Open Platform smart card (in this case, a JavaCard). To achieve these results, different biometric techniques have been studied: speaker verification, hand geometry and iris recognition. Experimental results are given to show the viability of the prototype developed     

基于离散单元法的二维颗粒阻尼研究

针对自由端带空腔的L型悬臂梁建立了二维颗粒阻尼物理模型,发展并利用离散单元法(DEM)对二维颗粒阻尼进行了数值仿真,重点考查了二维空腔尺寸对颗粒阻尼的影响规律:①高度非线性的颗粒阻尼能够显著地抑制结构振动,阻尼值至少比金属材料阻尼大一个数量级;②当无量纲加速度Γ<1时,颗粒阻尼很小;当Γ＞1时,随Γ增加,颗粒阻尼先增大...     

双面贴补层合板压缩屈曲渐进损伤分析

贴补复合材料层合板在压缩载荷作用下的屈曲破坏强度及其损伤演化过程对于复合材料结构修理具有重要意义。本文基于应变和黏聚区模型(CZM)建立了贴补复合材料层合板的渐进损伤分析模型,引入复合材料与胶层的损伤判据和刚度退化方案,计算了结构屈曲强度。数值仿真结果和实验数据吻合较好,验证了模型的有效性。基于该模型,采用非线性有限元方法研究了压缩载荷下双面贴补复合材料层合板的屈曲损伤演化过程,并讨论了补片参数对结构屈曲强度的影响。研究结果表明:双面贴补复合材料层合板屈曲后,处于拉伸和压缩状态下的铺层中的损伤程度存在差异;增大补片直径与厚度可以在一定程度上提高双面贴补复合材料层合板的屈曲强度。     

Thin Current Sheets in the Magnetotail Observed by Cluster

The dynamics of the current sheet is one of the most essential elements in magnetotail physics. Particularly, thin current sheets, which we define here as those with a thickness of less than several ion inertia lengths, are known to play an important role in the energy conversion process in the magnetotail. With its capability of multi-point observation, Cluster succeeded to obtain the current density continuously and therefore identify structures of thin current sheets. We discuss characteristics of the thin current sheets by showing their temporal evolution and the spatial structures based on several Cluster observations.     

Shock interactions in the outer heliosphere

Observations of plasma and magnetic fields by Pioneer 10 and 11 and Voyager 1 and 2 reveal that MHD shocks are an important component of the large-scale solar wind structures in the outer heliosphere. This review discusses recent progress in simulation studies of the nonlinear evolution of the solar wind structures, and in particular concentrates on the theoretical development and applications of the shock interactions model. Various stream propagation models, which do not use the Rankine-Hugoniot relations to calculate the jump conditions at shock crossings, have been used to simulate the essential evolution process of isolated streams and the formation and propagation of corotating and transient shocks. They produce fairly good results in the region up to a few AU. In 1984, the shock interactions model was introduced to study the evolution of large-scale solar wind structures in the region outside 1 AU up to several tens of AU. The model uses the exact Rankine-Hugoniot relations to calculate the shock speed and shock strength at all shock crossings. So that the model can more accurately calculate the shock speeds and the accumulated irreversible shock heating of plasma at several tens of AU. The applications of the shock interactions model are presented in three groups. (a) The first group covers the basic interaction of a shock with the ambient solar wind, the formation and propagation of shock pairs, and the collision and merging of shocks. (b) The second group covers the use of the shock interactions model to simulate the nonlinear evolution of large-scale solar wind structures in the outer heliosphere. These simulation results can provide the detailed evolution process for large-scale solar wind structures in the vast region not directly observed. Two selected studies are reported. (c) Finally, the shock interactions model is applied to studying the heating of the solar wind in the outer heliosphere. The model calculations support shocks being chiefly responsible for the heating of the solar wind plasma in the outer heliosphere at least up to 30 AU.     

Magnetic Fields in Astrophysical Jets: From Launch to Termination

Long-lived, stable jets are observed in a wide variety of systems, from protostars, through Galactic compact objects to active galactic nuclei (AGN). Magnetic fields play a central role in launching, accelerating, and collimating the jets through various media. The termination of jets in molecular clouds or the interstellar medium deposits enormous amounts of mechanical energy and momentum, and their interactions with the external medium, as well, in many cases, as the radiation processes by which they are observed, are intimately connected with the magnetic fields they carry. This review focuses on the properties and structures of magnetic fields in long-lived jets, from their launch from rotating magnetized young stars, black holes, and their accretion discs, to termination and beyond. We compare the results of theory, numerical simulations, and observations of these diverse systems and address similarities and differences between relativistic and non-relativistic jets in protostellar versus AGN systems. On the observational side, we focus primarily on jets driven by AGN because of the strong observational constraints on their magnetic field properties, and we discuss the links between the physics of these jets on all scales.     

Active Aerothermoelastic Control of Hypersonic Double-wedge Lifting Surface

Designing re-entry space vehicles and high-speed aircraft requires special attention to the nonlinear thermoelastic and aerodynamic instability of their structural components. The thermal effects are important since temperature environment brings dramatic influences on the static and dynamic behaviors of flight structures in supersonic/hypersonic regimes and is likely to cause instability, catastrophic failure and oscillations resulting in structural failure due to fatigue. In order to understand the dynamic behaviors of these ＂hot＂ structures, a double-wedge lifting surface with combining freeplay and cubic structural nonlinearities in both plunging and pitching degrees-of-freedom operating in supersonic/hypersonic flight speed regimes has been analyzed. A third order piston theory aerodynamic is used to estimate the applied nonlinear unsteady aerodynamic loads. Also considered is the loss of torsional stiffness that may be incurred by lifting surfaces subject to axial stresses induced by aerodynamic heating. The aerodynamic heating effects are estimated based on the adiabatic wall temperature due to high speed airstreams. As a recently emerging technology, the active aerothermoelastic control is aimed at providing solutions to a large number of problems involving the aeronautical/aerospace flight vehicle structures. To prevent such damaging phenomena from occurring, an application of linear and nonlinear active control methods on both flutter boundary and post-flutter behavior has been fulfilled. In this paper, modeling issues as well as numerical simulation have been presented and pertinent conclusions outlined. It is evidenced that a serious loss of torsional stiffness may induce the dynamic instability; however active control can be used to expand the flutter boundary and convert unstable limit cycle oscillations （LCO） into the stable LCO and/or to shift the transition between these two states toward higher flight Mach numbers.     

Corotating Interaction Regions in the Outer Heliosphere

We discuss the structure and evolution of CIRs and their successors in the outer heliosphere. These structures undergo significant evolution as they are convected to greater heliocentric distances. A progression of different types of structure are observed at increasing distance from the Sun. Similar structures are observed at similar heliocentric distance at different portions of the solar cycle. CIRs and their successors are associated with many important physical processes in the outer heliosphere. We discuss the relationship between these structures and recurrent phenomena such as cosmic ray variations, and review some of the associated theoretical models on the role of corotating structures and global merged interaction regions (GMIRs) in global cosmic ray modulation. We also discuss some outstanding questions related to the origin of non-dispersive quasi-periodic particle enhancements associated with CIRs and their successors in the outer heliosphere. This revised version was published online in August 2006 with corrections to the Cover Date.     

层流边界层C型失稳研究

本文研究了在平板层流边界层中，一个二维基本波和一对三维亚谐斜波的非线性作用，利用修正的弱非线性理论求出这些波的幅值、幅角的演化方程。文中主要观点是：高次谐波的能量不能瞬时被激发，而是由低次谐波通过非线性作用逐步产生的。本文积分有关方程，计算出基本波和亚谐斜波的参数，得到一段扰动演化曲线，与实验吻合较好。     

测压孔径对下沉安装压力传感器测量的影响

对于高超声速飞行试验,飞行器在飞行过程中产生的气动加热会使其表面安装的传感器烧坏并导致试验测量失败。传感器下沉安装可以避免其与飞行器周围的高温气体直接接触,减轻传感器的热载荷。采用下沉安装传感器的方式对高超声速边界层的脉动压力进行了试验测量,研究了测压孔径对脉动压力特性的影响。结果表明,随着孔径增大,脉动压力强度减小,流场相关性增强。传感器下沉安装会引起空腔流动,随着孔径的增大,空腔流动对脉动压力测量的影响降低。在频带10~20 kHz范围内,测压孔径仅仅影响脉动压力强度,在频带1~10 kHz范围内,测压孔径对脉动压力波形周期的影响更为显著。非线性耦合将能量由高频小尺度向低频大尺度传递,导致发生自相互作用和非线性相位耦合的流动结构趋向低频,随着孔径增大,非线性相位耦合消失。此外,孔径越大,不同尺度结构的能量分布与齐平安装的相似性越高。     

Compressible Aspects of Slow Solar Wind Formation

Recently we have shown how the slow solar wind can be formed within a coronal helmet streamer. The solar wind is modeled by a "wake-neutral" sheet, whose subsequent linear and nonlinear evolution provides clues to the development of the wind. In this paper we describe the first results of our extension of this model to the compressible regime. In particular, we show that traveling density enhancements are formed, similar to those observed by LASCO. The compressible equations are solved by an extension to MHD of the SPECLS algorithm. This revised version was published online in June 2006 with corrections to the Cover Date.     

Acceleration sensors based modal identification and active vibration control of flexible smart cantilever plate

Some flexible appendages of spacecrafts, such as solar panels, are cantilever plate structures. Thus, vibration problem is unavoidable when there is slewing maneuver or external disturbance excitation. Vibration of such cantilever plate structures includes coupled bending and torsional motion. Furthermore, the low amplitude vibration near the equilibrium point is very difficult to be quickly suppressed due to nonlinear factors of the hardware in the system, which is harmful to stability and attitude control accuracy. To solve these problems, acceleration sensor-based modal identification and active vibration control methods are presented for the first two bending and the first two torsional modes vibration of the cantilever plate. Optimal placements of three acceleration sensors and PZT patches actuators are performed to decouple the bending and torsional vibration of such cantilever plate for sensing and actuating, and identifications are achieved by experiments. A nonlinear control method is presented to suppress both high and low amplitude vibrations of flexible smart cantilever plate significantly. Experimental comparison researches are conducted by using acceleration proportional feedback and the presented nonlinear control algorithms. The experimental results demonstrate that the presented acceleration sensor-based methods can suppress the vibration of cantilever plate effectively.     

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.