Resonantly Excited Non-linear Density Waves in Disk Systems

Most of the disk systems are characterized by spiral structures. A good portion of these spiral structures can be identified as waves resonantly excited by a perturber in or pertaining to the same system. For planetary rings, this is an exterior satellite; for galactic disks, a rotating bar; for proto-stellar disks (yet to be confirmed), this would be a proto-planet. These waves, not just responsible for the present morphology of the disks, also play a dominating role on evolution of the disks. Resonance excitation is a extremely effective mechanism. A relatively weak perturbation can result in a highly non-linear responses in the disk. Therefore, non-linear theory is a necessity here. We will examine the non-linear theory of resonance excitation and discuss the applications of the theory to Saturn's rings and disk galaxies in this paper.     

层叠纤维增强板的振动问题

 本文用任意正交铺层的简支矩形板自由振动问题的精确解,通过计算研究了经典层板和考虑剪切的层板振动理论的适用范围;还研究了在经典层板横向振动理论中板平面内两个方向惯性力的影响问题,结论是可以忽略这种影响。     

VSAR: a high resolution radar system for ocean imaging

The velocity synthetic aperture radar (VSAR) is a conceptual synthetic aperture radar (SAR)-based sensor system for high resolution ocean imaging. The VSAR utilizes data collected by a multielement SAR system, to extract information not only about the radar reflectivity of the observed area, but also about the radial velocity of the scatterers in each pixel. This is accomplished by making use of the phase information contained in multiple SAR images, and not just the magnitude information as in conventional SAR. Using this velocity information, the VSAR attempts to compensate for the velocity distortion inherent in conventional SAR and to reconstruct the ocean reflectivity. We present the basic theory of the VSAR system and its performance. We also provide an analysis of the VSAR imaging mechanism for a statistical model of the radar returns, designed to capture the effects of speckle and of resolution degradation due to the decorrelation of the radar returns     

Pickup Ion Acceleration at the Termination Shock and in the Heliosheath

We discuss pickup ion acceleration and transport near the solar wind termination shock from the perspective of their spectral, spatial, and pitch-angle distributions. Our study is performed in the framework of a recently developed anisotropic transport model based on a Legendre polynomial expansion technique. Voyager 1 LECP angular distributions of 1 MeV protons, represented in the form of an expansion in spherical harmonics in the frame aligned with the measured interplanetary magnetic field, are used as benchmarks for our theory. We find the observed distributions consistent with our model predictions for particle acceleration and reflection at a highly oblique shock wave. It is shown that first-order (field aligned) anisotropy is a measure of shock obliquity while the second-order (transverse) anisotropy reflects the energy dependence of the particle scattering mean free path. We also discuss the role of enhanced scattering and momentum diffusion on the spectral properties of energetic charged particles.     

A comparison between observed and predicted mass-loss rates and wind momentum of O stars

Empirical mass-loss rates were derived for 28 luminous O stars from radio fluxes and H equivalent widths. Comparison with theoretical values predicted by the theory of radiatively driven winds reveals a discrepancy of 0.30±0.05 dex, with the theoretical values being too low. We show that there is not only a mass-loss discrepancy but also a momentum flux discrepancy. The theoretically predicted momentum fluxes are too low by 0.17±0.04 dex. This discrepancy is independent of the adopted stellar mass. We demonstrate that the momentum discrepancy in the most luminous O stars is comparable to the one found in the least extreme Wolf-Rayet stars. We suggest that the physical reason for the break-down of the theory in Wolf-Rayet stars and the most luminous O stars may be related.     

An Introduction to Theory and Models of CMEs, Shocks, and Solar Energetic Particles

We present a brief introduction to the essential physics of coronal mass ejections as well as a review of theory and models of CME initiation, solar energetic particle (SEP) acceleration, and shock propagation. A brief review of the history of CME models demonstrates steady progress toward an understanding of CME initiation, but it is clear that the question of what initiates CMEs has still not been solved. For illustration, we focus on the flux cancellation model and the breakout model. We contrast the similarities and differences between these models, and we examine how their essential features compare with observations. We review the generation of shocks by CMEs. We also outline the theoretical ideas behind the origin of a gradual SEP event at the evolving CME-driven coronal/interplanetary shock and the origin of “impulsive” SEP events at flare sites of magnetic reconnection below CMEs. We argue that future developments in models require focused study of “campaign events” to best utilize the wealth of available CME and SEP observations.     

关于几种特殊矩阵逆的求法

在n阶方阵求逆的方法上,研究了三类特殊矩阵逆的求法,不仅丰富了矩阵逆理论的内容,而且方便了矩阵论在运筹学、控制论以及工程领域中的应用。     

产业安全问题研究——基于生态学视角

随着中国对外开放程度不断加大,产业安全问题越来越引起人们的重视,但目前普遍采用的产业安全评价指标尚存在着片面性。文章通过运用生态系统健康评价理论来考察国家产业安全存在的问题和面临的挑战,认为国家产业系统是一个由各行业企业与环境构成的社会生态系统,也具有生态系统的一般属性,因而把生态学原理应用到产业安全问题研究上,借鉴生态系统安全理论提出了产业生态系统的内涵,构建了产业安全的健康指数和敏感性指标,为产业安全评价提供了新的思路与方法。     

Understanding the Dynamics of Magnetic Reconnection Layer

We review progress in understanding the dynamics of a typical magnetic reconnection layer by describing the historical development of theory and the recent findings and discoveries in space and laboratory plasmas. The emphasis is on the dynamics of electrons moving with respect to ions in the collision-free neutral sheet. We make a detailed comparison of experimental results from the Magnetic Reconnection Experiment (MRX) with those from theory and numerical simulations. The collaboration between space and laboratory scientists on reconnection research has recently reached a point where we can compare measurements of the reconnection layer profile in detail with support from numerical simulations. In spite of the large difference in physical scales by 10⁶?C10⁷, we find remarkable commonalities in the features of the magnetic reconnection region in laboratory and magnetospheric plasmas. A newly planned laboratory experiment, in which a current sheet is swept in the way a magnetosphere current sheet crosses space satellites, is also described.     

Notes on Magnetohydrodynamics of Magnetic Reconnection in Turbulent Media

Astrophysical fluids have very large Reynolds numbers and therefore turbulence is their natural state. Magnetic reconnection is an important process in many astrophysical plasmas, which allows restructuring of magnetic fields and conversion of stored magnetic energy into heat and kinetic energy. Turbulence is known to dramatically change different transport processes and therefore it is not unexpected that turbulence can alter the dynamics of magnetic field lines within the reconnection process. We shall review the interaction between turbulence and reconnection at different scales, showing how a state of turbulent reconnection is natural in astrophysical plasmas, with implications for a range of phenomena across astrophysics. We consider the process of magnetic reconnection that is fast in magnetohydrodynamic (MHD) limit and discuss how turbulence—both externally driven and generated in the reconnecting system—can make reconnection independent on the microphysical properties of plasmas. We will also show how relaxation theory can be used to calculate the energy dissipated in turbulent reconnecting fields. As well as heating the plasma, the energy dissipated by turbulent reconnection may cause acceleration of non-thermal particles, which is briefly discussed here.     

Transition prediction and sensitivity analysis for a natural laminar flow wing glove flight experiment

Natural laminar flow technology can significantly reduce aircraft aerodynamic drag and has excellent technical appeal for transport aircraft development with high aerodynamic efficiency. Accurately and efficiently predicting the laminar-to-turbulent transition and revealing the maintenance mechanism of laminar flow in a transport aircraft’s flight environment are significant for developing natural laminar flow wings. In this research, we carry out natural laminar flow flight experiments with different Reynolds numbers and angles of attack. The critical N-factor is calibrated as 9.0 using flight experimental data and linear stability theory from a statistical perspective, which makes sure that the relative error of transition location is within 5%. We then implement a simplified e^N transition prediction method with a similar accuracy compared with linear stability theory. We compute the sensitivity information for the simplified e^N method with an adjoint-based method, using the automatic differentiation technique (ADjoint). The impact of Reynolds numbers and pressure distributions on TS waves is analyzed using the sensitivity information. Through the sensitivity analysis, we find that: favorable pressure gradients not only suppress the development of TS waves but also decrease their sensitivity to Reynolds numbers; there exist three special regions which are very sensitive to the pressure distribution, and the sensitivity decreases as the local favorable pressure gradient increases. The proposed sensitivity analysis method enables robust natural laminar flow wings design.     

Particle Acceleration in Impulsive Solar Flares

We present the major observationally-derived requirements for a solar flare particle acceleration mechanism, briefly discuss some general electrodynamic constraints that also need to be considered, and suggest a unified electron and ion acceleration theory. This theory consists of two elements: cascading MHD turbulence generated at large scales during the primary flare energy release, which is responsible for the energization of electrons and all ions except 3He, and an electron beam, which excites the waves necessary for 3He acceleration. An issue of special importance for understanding ion acceleration is the convincing measurement of the charge state of Fe, which can be accomplished by the Advanced Composition Explorer in the upcoming solar maximum. This revised version was published online in June 2006 with corrections to the Cover Date.     

基于动态逆的综合非线性飞行控制方法

在解决非线性飞行控制问题中,动态逆控制方法已成为一种流行的控制方法.文中以动态逆控制方法为基础,使用神经网络控制与动态非线性阻尼控制综合的控制方法进行补偿,以提高非线性飞控系统的鲁棒性.在以某型推力矢量飞机为对象的仿真中,这种方法显示出很强的非线性控制能力和鲁棒性.     

用定量方法研究材料的断裂

本文简述了定量断口学的发展过程，说明了ＲＬ与ＲＳ的局限性。详细论述了分形几何作为一种新理论在断口分析中的应用，并提出了该领域目前存在的问题及努力方向。     

Low-Frequency Waves and Instabilities in Collisionless Plasmas

We present a theoretical overview of low-frequency waves and instabilities in collisionless, multi-component plasmas with gyrotropic ( ) thermal pressure. We show that the complete dispersion relation can be obtained in the framework of a mixed magnetohydrodynamic (MHD)-kinetic formalism, which uses the MHD mass, momentum, and induction equations, together with the kinetically corrected version of the double-adiabatic equations of state. The complete dispersion relation contains not only the three standard modes (fast, slow, and Alfvén) from double-adiabatic MHD, but also the mirror mode from kinetic theory. We examine the stability properties of these four modes, firstly in the case of a uniform medium, and secondly in the case of a stratified and rotating medium. We also discuss the connections with the quasi-interchange modes (interchange and translation) often referred to in the context of magnetospheric physics.     

Driving mechanisms for the solar wind

In this review, we consider the central physical aspects pertinent to the acceleration of the solar wind. Special importance is placed on the high-speed streams since the properties of these structures seem to strain the various theoretical explanations the most. Heavy emphasis is also given to the observations — particularly as to what constraints they place on the theories. We also discuss certain sporadic events such as spicules, macrospicules, X-ray bright points, and outflows seen in the EUV associated with the explosive events, jets, and coronal bullets which could be of relevance to this problem.Three theoretical concepts pertaining to the solar wind acceleration process are examined — purely thermal acceleration with and without extended heating, acceleration due to Alfvén wave pressure, and diamagnetic acceleration. Emphasis is given to how well these theories meet the constraints imposed by the observations. Diamagnetism is argued to be a powerful ingredient in solar wind theory, both in the light of observed sporatic outflows seen in the chromosphere and transition region and also because of its effectiveness in increasing the flow speed and producing strong acceleration near the Sun in line with coronal hole observations.     

企业合并商誉的确认与计量问题探讨

随着企业合并浪潮的高涨,企业合并商誉的确认和计量问题,已成为会计实务和理论界所关注的焦点.商誉的依附性、整体性、价值波动性等决定了其价值确切计量的难度较大.我国应在借鉴国外商誉会计处理理论和实践的基础上,结合我国商誉会计的现状,确认商誉,并选择适合我国国情的方法对合并商誉进行初始计量和后续计量.     

球状三嵌段共聚物在平面薄膜间的自组装

采用动态密度泛函理论（DDFT）对ABA型球状三嵌段共聚物在平板间的相行为进行了模拟研究。考查了不同强度的表面诱导对三嵌段共聚物自组装的影响。通过逐渐增大衬底作用,发现了多种偏离于本体的新结构,如浸润层相、平行柱状相、穿孔层相、层状相。发现浸润层相存在的表面场范围与短链的熵效应密切相关,同时熵效应的大小则依赖于长短链段的长度之比。在很多实际存在的嵌段共聚物中,如果在适当的实验条件下,应可以观察到模拟计算所预言的相结构。     

超声速气流中受热壁板的二次失稳型颤振

研究了超声速气流中受热壁板的非线性气动弹性响应,发现了一种新的动态失稳现象——二次失稳型颤振。基于von Karman非线性应变-位移关系、Reissner-Mindlin板理论和一阶活塞理论建立超声速气流中三维壁板的有限元模型。通过数值算例,研究了超声速气流中受热壁板发生二次失稳型颤振的条件,并运用非线性振动理论分析了二次失稳型颤振的机理。研究表明,超声速气流中受热壁板在平衡态的稳定性未发生变化时,也会因系统参数的变化引起气动弹性响应性质的突变,导致壁板的二次失稳型颤振。二次失稳型颤振能否发生不仅受到气流速压和壁板温升的影响,而且还与初始扰动有关。当扰动引起壁板的初始变形较小时,不能激发出二次失稳型颤振,壁板的气动弹性响应最终收敛到屈曲平衡态。应用二次失稳型颤振理论和分析方法,确定了前人给出的一个金属壁板模型的热颤振边界的风洞试验结果,而且计算结果与试验结果符合良好,从而对这一壁板热颤振现象的风洞试验结果作出了较合理的理论解释。