基于CFD的电磁散射数值模拟

计算流体力学(CFD)技术中的时域有限体积法(FVTD)被推广到计算电磁学中,直接数值求解时变麦克斯韦方程组.FVTD使用电磁场矢量共置于网格单元中心、散射场积分形式的麦克斯韦方程组守恒形,空间离散使用基于特征值的近似黎曼解构建网格单元边界通量,时间推进采用四阶龙格-库塔法.TM和TE波极化下几种二维完全导电体的表面诱导电流密度和雷达散射截面(RCS)计算验证表明,时域有限体积法是一种高精度有效的时域方法.     

Global Properties of Solar Flares

This article broadly reviews our knowledge of solar flares. There is a particular focus on their global properties, as opposed to the microphysics such as that needed for magnetic reconnection or particle acceleration as such. Indeed solar flares will always remain in the domain of remote sensing, so we cannot observe the microscales directly and must understand the basic physics entirely via the global properties plus theoretical inference. The global observables include the general energetics—radiation in flares and mass loss in coronal mass ejections (CMEs)—and the formation of different kinds of ejection and global wave disturbance: the type II radio-burst exciter, the Moreton wave, the EIT “wave”, and the “sunquake” acoustic waves in the solar interior. Flare radiation and CME kinetic energy can have comparable magnitudes, of order 10³² erg each for an X-class event, with the bulk of the radiant energy in the visible-UV continuum. We argue that the impulsive phase of the flare dominates the energetics of all of these manifestations, and also point out that energy and momentum in this phase largely reside in the electromagnetic field, not in the observable plasma.     

Now we can explore the Universe

It is suggested that the old scientific myth: “Nothing can go faster than light!” should be changed to: “Nothing electromagnetic can go faster than light!” Now that it is known that infinite velocity of propagation (VOP) is possible, there is another communications media whose VOP may be infinite. An experiment is under construction to compare electric field and electromagnetic transmission VOP. Since magnetic fields in electric field transmission will be parallel to the direction of transmission rather than at right angles, there is reason to expect that electric field transmissions will have infinite VOP     

Computational tools for supporting the testing of civil aircraft configurations in wind tunnels

Following a review of well-known CFD packages, this paper presents the mathematical and methodical ideas, which became the basis of the numerical method for a solution of the Reynolds (time)-averaged Navier–Stokes equations (RANS), relevant to supporting testing an aircraft configuration in wind tunnels (WTs). The estimation of finite speed of information propagation due to diffusion is given. Explicit and implicit methods for numerical solution of gasdynamic equations are compared. Stability conditions, taking into account both interaction of convection with diffusion and presence of exponentially varying modes of solution, are considered. Three methods of time stepping organization are described—global, local and fractional time stepping. Numerical boundary conditions for simulation of flow in the WT are proposed. Examples of method implementation for the European Transonic Windtunnel (ETW) case are presented.     

电弧喷射推力器电磁场模拟

为了揭示电弧喷射推力器内部电磁场特征及其与高温电离气体间的相互作用机理,建立了比较完善的电磁场模型,详细讨论了电磁场数值模拟方法及其计算效果.模型同时考虑了电场力、洛仑兹力和电子压强梯度对传导电流的贡献,由电子动力学方程和粒子微观碰撞理论推导出电流方程,由麦克斯韦方程组推导出电磁场控制方程,采用包括强隐过程(SIP)迭代法在内的十种迭代方法求解离散的电磁场方程.研究表明,SIP迭代法是适用于电弧喷射推力器电磁场模拟的快速有效的方法,模型能够准确地反映推力器内部电磁场与高温电离气体间的相互作用机理.     

Experimental Aspects of Mid-Frequency Pulsations (f≈10–100 mHz) in the Southern Polar Cap

We review the results obtained in the frequency range of Pc3 (22-100 mHz) and Pc4 (7-22 mHz) pulsations at Italian Antarctic stations in the southern polar cap (“Mario Zucchelli”, at Terra Nova Bay, TNB, 80^˚.S; “Concordia”, the Italian/French base at Dome C, DMC, 89^˚.S). The absence of a midnight enhancement in the pulsation power suggests a negligible substorm influence at extreme latitudes, while the sharp noon enhancement, which appears only at TNB, is determined by the closer proximity of the station to cusp related phenomena. The relationship between the frequency of the band-limited signals and the interplanetary magnetic field strength, the cone angle influence, and the higher correlation of the Pc3 power with the solar wind speed in the morning hours suggest a global scenario in which upstream waves would be mainly responsible for the mid-frequency activity in the polar cap. However, the polarization pattern is odd with respect to the predictions for tailward propagating modes.     

The radiation continuum model of light and the Galilean invarianceof Maxwell's equations

The original basis for the Lorentz transformations, and thus special relativity, was the assumption that the observed velocity of interaction of light with matter represents a unique velocity of the electromagnetic wave. This arbitrary decision is not borne out by Maxwell's theories or by any test that might prove that EM energy actually travels in a continuum of velocities. The second postulate as stated by Einstein does not deserve the status of a postulate, as it is at once overly restrictive and ultimately phenomenological-the nature of c is based on experimental measurement rather than on analysis of first principles. The radiation continuum model's (RCM) modified second postulate, however, says nothing about the actual propagation of EM energy, but only of the relative speed with which it must interact with matter to be detected. Utilizing this modified light principle we obtain an intuitive Galilean form invariance for Maxwell's equations. RCM places no upper limit on attainable velocities, and allows for the possibility of communications between humans or particles at speeds far in excess of c. This precludes many of the compatibility problems between the highly successful quantum mechanics and relativity theory     

Gravity Field Recovery from GRACE: Unique Aspects of the High Precision Inter-Satellite Data and Analysis Methods

The very high accuracy of the Doppler and range measurements between the two low-flying and co-orbiting spacecraft of the GRACE mission, which will be at the μm/sec and ≈10 μm levels respectively, requires that special procedures be applied in the processing of these data. Parts of the existing orbit determination and gravity field parameters retrieval methods and software must be modified in order to fully benefit from the capabilities of this mission. This is being done in the following areas: (i) numerical integration of the equations of motion (summed form, accuracy of the predictor-corrector loop, Encke's formulation): (ii) special inter-satellite dynamical parameterization for very short arcs; (iii) accurate solution of large least-squares problems (normal equations vs. orthogonal decomposition of observation equations); (iv) handling the observation equations with high accuracy. Theoretical concepts and first tests of some of the newly implemented algorithms are presented. This revised version was published online in August 2006 with corrections to the Cover Date.     

The Ultra Heavy Elements in the Cosmic Radiation

The concept that nuclei of all of the elements in the periodic table were accelerated to relativistic energies in the primary cosmic rays was confirmed by the discovery of the presence of nuclei significantly heavier than iron. These “ultra heavy” nuclei must all have been synthesized in endothermic reactions, occurring predominately in the final stages of stellar evolution. Determination of the relative abundances of these nuclei should provide new insights into the nuclear processes in some of the most energetic events in the life cycle of stars. The very low abundances of these nuclei relative to those of the exothermic lighter nuclei have made progress difficult. In addition, the effects of apparent preferential acceleration mechanisms and of propagation through the interstellar medium have distorted the source abundances. The history of the original discovery of the presence of these nuclei will be followed by a summary of the present state of knowledge of the observed abundances. The effects of acceleration biases and of interstellar propagation will be discussed. Finally some of the possibilities for further advances will be outlined. A copy of the Power Point presentation for this talk is available on request.     

Solar System Magnetospheres

This article proposes a short review of our present knowledge of solar system magnetospheres, with the purpose of placing the study of Saturn’s magnetosphere in the context of a comparative approach. We describe the diversity of solar system magnetospheres and the underlying causes of this diversity: nature and magnetization state of the planetary obstacle, presence or not of a dense atmosphere, rotation state of the planet, existence of a system of satellites, rings and neutral gas populations in orbit around the planet. We follow the “russian doll” hierarchy of solar system magnetospheres to briefly describe the different objects of this family: the heliosphere, which is the Sun’s magnetosphere; the “elementary” magnetospheres of the inner planets, Earth and Mercury; the “complex” magnetospheres of the giant planets, dominated by planetary rotation and the presence of interacting objects within their magnetospheric cavities, some of which, like Ganymede, Io or Titan, produce small intrinsic or induced magnetospheres inside the large one.We finally describe the main original features of Saturn’s magnetosphere as we see them after the Voyager fly-bys and before the arrival of Cassini at Saturn, and list some of the key questions which Cassini will have to address during its four-year orbital tour.     

Theory and Simulation of Reconnection

Reconnection is a major commonality of solar and magnetospheric physics. It was conjectured by Giovanelli in 1946 to explain particle acceleration in solar flares near magnetic neutral points. Since than it has been broadly applied in space physics including magnetospheric physics. In a special way this is due to Harry Petschek, who in 1994 published his ground breaking solution for a 2D magnetized plasma flow in regions containing singularities of vanishing magnetic field. Petschek’s reconnection theory was questioned in endless disputes and arguments, but his work stimulated the further investigation of this phenomenon like no other. However, there are questions left open. We consider two of them – “anomalous” resistivity in collisionless space plasma and the nature of reconnection in three dimensions. The CLUSTER and SOHO missions address these two aspects of reconnection in a complementary way -- the resistivity problem in situ in the magnetosphere and the 3D aspect by remote sensing of the Sun. We demonstrate that the search for answers to both questions leads beyond the applicability of analytical theories and that appropriate numerical approaches are necessary to investigate the essentially nonlinear and nonlocal processes involved. Necessary are both micro-physical, kinetic Vlasov-equation based methods of investigation as well as large scale (MHD) simulations to obtain the geometry and topology of the acting fields and flows.     

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.     

Implicit plasma simulation

Implicit time integration methods have been used extensively in numerical modelling of slowly varying phenomena in systems that also support rapid variation. Examples include diffusion, hydrodynamics and reaction kinetics. This article discusses implementation of implicit time integration in plasma codes of the “particle-in-cell” family, and the benefits to be gained.     

包含平均旋流的圆环管道声传播的模态分析

通过对三维线化欧拉方程的特征模态分析,研究包含平均旋流情况下声波在敷设声衬的圆环管道中的传播.特征模态分析采用谱配置方法计算轴向波数谱及扰动量的分布.当有平均旋流存在时,特征模态谱主要包括近/纯声模态和近/纯对流模态,旋流的存在甚至会改变传播模态个数,从而改变声波传播截止特性.在验证程序正确性的基础上,研究流动参数及声衬对声模态及对流模态的影响.      

Numerical modeling of large elastoplastic strains in terms of principal stretches. I. Kinematics of elastoplastic strains

A technique for numerical finite element analysis of large elastoplastic strains is proposed. A problem is formulated in terms of principal stretches and their logarithms in the current basis of the left distortion tensor. It is shown that the “classical” multiplicative decomposition of the total strain gradient into the product of elastic and plastic strain gradients is equivalent to the presentation of total stretches as a product of elastic and plastic stretches.     

A Model of the Magnetic Field Long-Term Evolution at the Coronal Base and Polar Heliospheric Regions

The long-term evolution of the polar magnetic field at the coronal base induced by the first Rossby mode demonstrates the reversal of the line-of-sight magnetic field component in polar caps and what is more the same line-of-sight magnetic polarities in both caps (“the line-of-sight solar magnetic monopole”) at the moment of reversal. This revised version was published online in August 2006 with corrections to the Cover Date.     

Clusters of Galaxies: Beyond the Thermal View

We present the work of an international team at the International Space Science Institute (ISSI) in Bern that worked together to review the current observational and theoretical status of the non-virialised X-ray emission components in clusters of galaxies. The subject is important for the study of large-scale hierarchical structure formation and to shed light on the “missing baryon” problem. The topics of the team work include thermal emission and absorption from the warm-hot intergalactic medium, non-thermal X-ray emission in clusters of galaxies, physical processes and chemical enrichment of this medium and clusters of galaxies, and the relationship between all these processes. One of the main goals of the team is to write and discuss a series of review papers on this subject. These reviews are intended as introductory text and reference for scientists wishing to work actively in this field. The team consists of sixteen experts in observations, theory and numerical simulations.     

DLR-F6翼身组合体的高阶精度数值模拟

基于雷诺平均Navier-Stokes(RANS)方程和结构网格技术,采用五阶空间离散精度的加权紧致非线性格式(WCNS)和剪切应力输运(SST)两方程湍流模型,开展了DLR-F6翼身组合体的高阶精度数值模拟研究。主要目的是确认WCNS模拟跨声速典型运输机构型的能力。采用粗、中、细3套网格开展了网格收敛性研究,从气动特性、压力分布、表面流态等方面研究了网格密度对DLR-F6翼身组合体气动特性的影响;采用中等网格开展了来流迎角对气动特性的影响研究。通过与试验数据、CFL3D软件和TRIP软件计算结果的对比,表明网格密度主要影响激波位置和压差阻力系数,同时对翼身结合部分离区大小有一定影响;采用高阶精度计算方法显著提高了气动力系数的模拟精度,力矩系数数值模拟结果与试验的差异有待进一步分析。     

Virtis: An Imaging Spectrometer for the Rosetta Mission

The VIRTIS (Visual IR Thermal Imaging Spectrometer) experiment has been one of the most successful experiments built in Europe for Planetary Exploration. VIRTIS, developed in cooperation among Italy, France and Germany, has been already selected as a key experiment for 3 planetary missions: the ESA-Rosetta and Venus Express and NASA-Dawn. VIRTIS on board Rosetta and Venus Express are already producing high quality data: as far as Rosetta is concerned, the Earth-Moon system has been successfully observed during the Earth Swing-By manouver (March 2005) and furthermore, VIRTIS will collect data when Rosetta flies by Mars in February 2007 at a distance of about 200 kilometres from the planet. Data from the Rosetta mission will result in a comparison – using the same combination of sophisticated experiments – of targets that are poorly differentiated and are representative of the composition of different environment of the primordial solar system. Comets and asteroids, in fact, are in close relationship with the planetesimals, which formed from the solar nebula 4.6 billion years ago. The Rosetta mission payload is designed to obtain this information combining in situ analysis of comet material, obtained by the small lander Philae, and by a long lasting and detailed remote sensing of the comet, obtained by instrument on board the orbiting Spacecraft. The combination of remote sensing and in situ measurements will increase the scientific return of the mission. In fact, the “in situ” measurements will provide “ground-truth” for the remote sensing information, and, in turn, the locally collected data will be interpreted in the appropriate context provided by the remote sensing investigation. VIRTIS is part of the scientific payload of the Rosetta Orbiter and will detect and characterise the evolution of specific signatures – such as the typical spectral bands of minerals and molecules – arising from surface components and from materials dispersed in the coma. The identification of spectral features is a primary goal of the Rosetta mission as it will allow identification of the nature of the main constituent of the comets. Moreover, the surface thermal evolution during comet approach to sun will be also studied.     

Quality analysis of nonlinear elasticity theory for the stability problems of planar laminated curved beams. Algorithm and results of numerical study

The algorithm of numerical solution for the linearized equations of the neutral equilibrium earlier constructed for the planar laminated curved beams is presented. The equations are based on the relations of the classical nonlinear theory of elasticity and the similar relations previously proposed in the consistent variant. We analyzed the results of numerical quality studies of the mentioned variants of nonlinear equations used when the linearized problems on possible buckling modes under the action of conservative forces and a stationary temperature field are formulated.