Solar Wind Turbulence and the Role of Ion Instabilities

Solar wind is probably the best laboratory to study turbulence in astrophysical plasmas. In addition to the presence of magnetic field, the differences with neutral fluid isotropic turbulence are: (i) weakness of collisional dissipation and (ii) presence of several characteristic space and time scales. In this paper we discuss observational properties of solar wind turbulence in a large range from the MHD to the electron scales. At MHD scales, within the inertial range, turbulence cascade of magnetic fluctuations develops mostly in the plane perpendicular to the mean field, with the Kolmogorov scaling $k_{\perp}^{-5/3}$ for the perpendicular cascade and $k_{\|}^{-2}$ for the parallel one. Solar wind turbulence is compressible in nature: density fluctuations at MHD scales have the Kolmogorov spectrum. Velocity fluctuations do not follow magnetic field ones: their spectrum is a power-law with a ?3/2 spectral index. Probability distribution functions of different plasma parameters are not Gaussian, indicating presence of intermittency. At the moment there is no global model taking into account all these observed properties of the inertial range. At ion scales, turbulent spectra have a break, compressibility increases and the density fluctuation spectrum has a local flattening. Around ion scales, magnetic spectra are variable and ion instabilities occur as a function of the local plasma parameters. Between ion and electron scales, a small scale turbulent cascade seems to be established. It is characterized by a well defined power-law spectrum in magnetic and density fluctuations with a spectral index close to ?2.8. Approaching electron scales, the fluctuations are no more self-similar: an exponential cut-off is usually observed (for time intervals without quasi-parallel whistlers) indicating an onset of dissipation. The small scale inertial range between ion and electron scales and the electron dissipation range can be together described by $\sim k_{\perp}^{-\alpha}\exp(-k_{\perp}\ell_{d})$ , with α?8/3 and the dissipation scale ? _d close to the electron Larmor radius ? _d ?ρ _e . The nature of this small scale cascade and a possible dissipation mechanism are still under debate.     

Observations of Magnetospheric Waves and their Relation to Precipitation

Magnetospheric wave observations are discussed from the viewpoint of their potential importance for precipitation of charged particles into the auroral zones. While wave processes are a fundamental part of magnetospheric plasma physics, occurring most of the time in most of the magnetospheric regions, their direct role in and relative importance for auroral precipitation are not easy to assess. The role of the waves varies from one spatial region to another and is very different for electrons and ions. Furthermore, the distinction between wave processes and other precipitation mechanisms is not at all straightforward. This review focuses on four main topics: The problem of diffuse electron precipitation, the recent surprise on the detailed structure of broad-banded electrostatic noise in the plasma sheet boundary layer, ion precipitation through electromagnetic ion cyclotron waves, and the role of low-altitude waves in precipitation. It is concluded that, while the observational status of high-altitude ion cyclotron waves is reasonably good, in most areas more thorough studies of existing data as well as refined observations are very much needed. Successful observational studies are to be carried out jointly with theoretical work as well as with studies on the large-scale context of the often localized wave processes. This is especially important when interests are moving toward more nonlinear phenomena, such as shocks, double layers, or strong quasi-static gradients, where a strict adherence to classical wave concepts is becoming more and more diffuse and less motivated.     

涡轮叶片来流角扰动不确定性量化分析

为了高效精确量化来流条件变化对涡轮叶片性能的影响,发展了一种基于自适应抽样技术的非嵌入式多项式混沌(NIPC)模型,并通过函数试验对自适应NIPC模型进行了验证。在不同尺度来流角变化下,用该模型量化涡轮叶栅能量损失系数的不确定性变化,同时与直接蒙特卡洛模拟和灵敏度分析进行对比。通过流场统计分析揭示来流角变化对气动不确定性的影响机理。结果表明:自适应NIPC在不同尺度来流角扰动下均能快速准确量化能量损失系数变化;能量损失系数不确定性变化对来流角扰动是非线性依赖关系;叶片通道内的激波对来流角变化最为敏感,是引起能量损失系数不确定性变化的主要因素。     

磁流体湍流中的结构和能量传输

磁流体湍流中存在多种相干结构,包括电流和涡旋结构。文章主要对近几年有关磁流体湍流相干结构及其相关的能量传输的一些工作进行了介绍。不同于中性流体湍流中的管状结构,磁流体中的相干结构多呈现为片状,强电流片附近也存在强涡片结构。磁流体湍流中的能量级串使能量跨尺度从大尺度传递至小尺度;与中性流体湍流能量传输主要集中在相近尺度上不同,磁流体湍流除了动能传输,还有磁能传输,以及动能与磁能之间的跨尺度互相转换。研究表明,磁流体湍流中的能量传输及耗散具有强间歇性,集中在较小区域范围,且与相干结构存在关联。在存在背景磁场的情况下,磁流体湍流中的相干结构在背景磁场方向上被拉长,而同样方向上的能量传输受到抑制。在高马赫数的情况下,激波的产生会使能量传输明显增强,同时带来很强的间歇性,结构函数标度律远远偏离线性标度关系,并且随着阶数的增加,标度指数会达到饱和值。     

Coupling from the Photosphere to the Chromosphere and the Corona

The atmosphere of the Sun is characterized by a complex interplay of competing physical processes: convection, radiation, conduction, and magnetic fields. The most obvious imprint of the solar convection and its overshooting in the low atmosphere is the granulation pattern. Beside this dominating scale there is a more or less smooth distribution of spatial scales, both towards smaller and larger scales, making the Sun essentially a multi-scale object. Convection and overshooting give the photosphere its face but also act as drivers for the layers above, namely the chromosphere and corona. The magnetic field configuration effectively couples the atmospheric layers on a multitude of spatial scales, for instance in the form of loops that are anchored in the convection zone and continue through the atmosphere up into the chromosphere and corona. The magnetic field is also an important structuring agent for the small, granulation-size scales, although (hydrodynamic) shock waves also play an important role—especially in the internetwork atmosphere where mostly weak fields prevail. Based on recent results from observations and numerical simulations, we attempt to present a comprehensive picture of the atmosphere of the quiet Sun as a highly intermittent and dynamic system.     

Upstream Ion Cyclotron Waves at Venus and Mars

The occurrence of waves generated by pick-up of planetary neutrals by the solar wind around unmagnetized planets is an important indicator for the composition and evolution of planetary atmospheres. For Venus and Mars, long-term observations of the upstream magnetic field are now available and proton cyclotron waves have been reported by several spacecraft. Observations of these left-hand polarized waves at the local proton cyclotron frequency in the spacecraft frame are reviewed for their specific properties, generation mechanisms and consequences for the planetary exosphere. Comparison of the reported observations leads to a similar general wave occurrence at both planets, at comparable locations with respect to the planet. However, the waves at Mars are observed more frequently and for long durations of several hours; the cyclotron wave properties are more pronounced, with larger amplitudes, stronger left-hand polarization and higher coherence than at Venus. The geometrical configuration of the interplanetary magnetic field with respect to the solar wind velocity and the relative density of upstream pick-up protons to the background plasma are important parameters for wave generation. At Venus, where the relative exospheric pick-up ion density is low, wave generation was found to mainly take place under stable and quasi-parallel conditions of the magnetic field and the solar wind velocity. This is in agreement with theory, which predicts fast wave growth from the ion/ion beam instability under quasi-parallel conditions already for low relative pick-up ion density. At Mars, where the relative exospheric pick-up ion density is higher, upstream wave generation may also take place under stable conditions when the solar wind velocity and magnetic field are quasi-perpendicular. At both planets, the altitudes where upstream proton cyclotron waves were observed (8 Venus and 11 Mars radii) are comparable in terms of the bow shock nose distance of the planet, i.e. in terms of the size of the solar wind-planetary atmosphere interaction region. In summary, the upstream proton cyclotron wave observations demonstrate the strong similarity in the interaction of the outer exosphere of these unmagnetized planets with the solar wind upstream of the planetary bow shock.     

Stimulated electromagnetic emissions by high-frequency electromagnetic pumping of the ionospheric plasma

A high frequency electromagnetic pump wave transmitted into the ionospheric plasma from the ground can stimulate electromagnetic radiation with frequencies around that of the ionospherically reflected pump wave. The numerous spectral features of these stimulated electromagnetic emissions (SEE) and their temporal evolution on a wide range of time scales are reviewed and related theoretical, numerical, and simulation results are discussed. On long (thermal) time scales the SEE constitutes a self-organization of the ionospheric plasma which depends on the interaction of nonlinear processes in a hierarchy of time scales in response to the electromagnetic pumping. Particularly, the appearance of the rich SEE spectrum is associated with the slow self-structuring of the plasma density into a spectrum of magnetic field-aligned density striations. The dependence of the SEE on electron gyroharmonic effects and the presence of density striations suggests that the existence of a magnetic field in the plasma is important for plasma turbulence to dissipate into non-thermal electromagnetic radiation during the long time quasi-stationary state of the turbulence evolution.     

Cyclotron Resonant Interactions in Cosmic Particle Accelerators

A review is given for cyclotron resonant interactions in space plasmas. After giving a simple formulation for the test particle approach, illustrative examples for resonant interactions are given. It is shown that for obliquely propagating whistler waves, not only fundamental cyclotron resonance, but also other resonances, such as transit-time resonance, anomalous cyclotron resonance, higher-harmonic cyclotron resonance, and even subharmonic resonance can come into play. A few recent topics of cyclotron resonant interactions, such as electron injection in shocks, cyclotron resonant heating of solar wind heavy ions, and relativistic modifications, are also reviewed.     

Nonclassical Transport and Particle-Field Coupling: from Laboratory Plasmas to the Solar Wind

Understanding transport of thermal and suprathermal particles is a fundamental issue in laboratory, solar-terrestrial, and astrophysical plasmas. For laboratory fusion experiments, confinement of particles and energy is essential for sustaining the plasma long enough to reach burning conditions. For solar wind and magnetospheric plasmas, transport properties determine the spatial and temporal distribution of energetic particles, which can be harmful for spacecraft functioning, as well as the entry of solar wind plasma into the magnetosphere. For astrophysical plasmas, transport properties determine the efficiency of particle acceleration processes and affect observable radiative signatures. In all cases, transport depends on the interaction of thermal and suprathermal particles with the electric and magnetic fluctuations in the plasma. Understanding transport therefore requires us to understand these interactions, which encompass a wide range of scales, from magnetohydrodynamic to kinetic scales, with larger scale structures also having a role. The wealth of transport studies during recent decades has shown the existence of a variety of regimes that differ from the classical quasilinear regime. In this paper we give an overview of nonclassical plasma transport regimes, discussing theoretical approaches to superdiffusive and subdiffusive transport, wave–particle interactions at microscopic kinetic scales, the influence of coherent structures and of avalanching transport, and the results of numerical simulations and experimental data analyses. Applications to laboratory plasmas and space plasmas are discussed.     

Damping Mechanisms for Oscillations in Solar Prominences

Small amplitude oscillations are a commonly observed feature in prominences/filaments. These oscillations appear to be of local nature, are associated to the fine structure of prominence plasmas, and simultaneous flows and counterflows are also present. The existing observational evidence reveals that small amplitude oscillations, after excited, are damped in short spatial and temporal scales by some as yet not well determined physical mechanism(s). Commonly, these oscillations have been interpreted in terms of linear magnetohydrodynamic (MHD) waves, and this paper reviews the theoretical damping mechanisms that have been recently put forward in order to explain the observed attenuation scales. These mechanisms include thermal effects, through non-adiabatic processes, mass flows, resonant damping in non-uniform media, and partial ionization effects. The relevance of each mechanism is assessed by comparing the spatial and time scales produced by each of them with those obtained from observations. Also, the application of the latest theoretical results to perform prominence seismology is discussed, aiming to determine physical parameters in prominence plasmas that are difficult to measure by direct means.     

柯恩达效应对涡轮叶栅气动性能及流场的影响

以某实际燃气轮机涡轮进口导向器叶栅为研究对象,在出口为高亚声速及超声速条件下,对具有不同柯恩达表面的环量控制叶栅进行二维数值模拟,通过对比分析叶栅的气动性能和流场细节,探讨了柯恩达效应在涡轮叶栅中的作用机理.结果表明:当叶栅出口马赫数为0.60时,射流对主流有很好的携带作用,损失小于原型叶栅;叶栅出口马赫数增加到0.85时,射流仍有较强的携带主流折转的能力;当叶栅出口为超声速时,在初始阶段小曲率的柯恩达表面上,由于激波的作用,射流向流道中心折转并提前脱离壁面,初始阶段大曲率的柯恩达表面射流附壁较好,但由于叶片吸力面与射流口之间圆角的作用,射流与主流掺混不理想.      

Topics in Microphysics of Relativistic Plasmas

Astrophysical plasmas can have parameters vastly different from the more studied laboratory and space plasmas. In particular, the magnetic fields can be the dominant component of the plasma, with energy-density exceeding the particle rest-mass energy density. Magnetic fields then determine the plasma dynamical evolution, energy dissipation and acceleration of non-thermal particles. Recent data coming from astrophysical high energy missions, like magnetar bursts and Crab nebula flares, point to the importance of magnetic reconnection in these objects. In this review we outline a broad spectrum of problems related to the astrophysical relevant processes in magnetically dominated relativistic plasmas. We discuss the problems of large scale dynamics of relativistic plasmas, relativistic reconnection and particle acceleration at reconnecting layers, turbulent cascade in force-fee plasmas. A number of astrophysical applications are also discussed.     

Current Status of Turbulent Dynamo Theory

Several recent advances in turbulent dynamo theory are reviewed. High resolution simulations of small-scale and large-scale dynamo action in periodic domains are compared with each other and contrasted with similar results at low magnetic Prandtl numbers. It is argued that all the different cases show similarities at intermediate length scales. On the other hand, in the presence of helicity of the turbulence, power develops on large scales, which is not present in non-helical small-scale turbulent dynamos. At small length scales, differences occur in connection with the dissipation cutoff scales associated with the respective value of the magnetic Prandtl number. These differences are found to be independent of whether or not there is large-scale dynamo action. However, large-scale dynamos in homogeneous systems are shown to suffer from resistive slow-down even at intermediate length scales. The results from simulations are connected to mean field theory and its applications. Recent work on magnetic helicity fluxes to alleviate large-scale dynamo quenching, shear dynamos, nonlocal effects and magnetic structures from strong density stratification are highlighted. Several insights which arise from analytic considerations of small-scale dynamos are discussed.     

不同周向位置端壁翼刀对压气机叶栅损失影响的实验研究

在低速大尺寸叶栅风洞上通过详细测量叶栅流场,研究了叶栅端壁上不同周向位置处加装端壁翼刀对压气机叶栅损失和二次流的影响。实验结果表明,合理选择翼刀安装位置,可有效地控制压气机叶栅的二次流,降低叶栅的总损失。进一步对实验方案中叶栅总损失最小的翼刀位置的叶栅内流场进行了测量,分析了安装翼刀后流场内涡系结构的变化,探讨了翼刀涡的形成和发展变化。      

激光增材制造过程数值仿真技术综述

数值仿真是研究激光增材制造过程中各类物理现象、揭示零件缺陷形成机理、优化增材制造工艺参数的重要手段,该领域学者针对增材制造过程中的热分析、金属粉末颗粒性质分析、微观结构分析、质量缺陷成因分析等方面,开展了大量研究,提出了相应的数学模型和方法。激光增材制造过程的数值仿真是一个在空间和时间上均跨越多个尺度的复杂问题,微观、介观、宏观尺度下数值仿真所关注的对象和所使用的方法各不相同;多数研究聚焦于某一尺度下的过程仿真,另一部分研究则基于不同模型的数据关系建立模型间的耦合关系,实现热-相、热-力的综合分析。对现阶段激光增材制造数值仿真领域的主要技术进行了综述,在梳理数值仿真基本流程的基础上,对其中涉及的热源模型,粉末模型,力学模型以及微观结构模型进行了介绍,讨论了其特点和适用性;结合相关技术领域的发展,探讨了激光增材制造数值仿真技术的发展方向,旨在为本领域的技术研究与发展提供参考。     

Influences of meridional flowpath on the performance of swept blade in an axial compressor stage

A series of numerical simulations were conducted in both a 1.5 stage axial compressor model and a simplified planar cascade model. The cases with different blade sweep schemes in the cascade model were simulated with free-slip endwalls to minimize the influence of endwall 3-D(three-dimensional) flows. The results obtained in the cascade model were discussed at first for getting a clear insight into the effects of blade sweep without other influences. And then the simulation results of the 1.5 stage compressor model were discussed accordingly. The discussions focused on the influences of different meridional flowpath designs, i.e. constant mid radius (CMR) design, constant outer radius (COR) design and constant inner radius (CIR) design, on the performance of the swept blade. The results showed that the most critical effect produced by blade sweep was attributed to the redistribution of local mass-flow-rate in blade spanwise direction. The change of meridional flowpath did not change the mass-flow-rate redistribution behaviors. However, the trends for local mass-flow-rate redistribution in compressor stage model showed some discrepancies compared with the results shown in the planar cascade model.      

Environments in the Outer Solar System

The outer planets of our solar system Jupiter, Saturn, Uranus, and Neptune are fascinating objects on their own. Their intrinsic magnetic fields form magnetic environments (so called magnetospheres) in which charged and neutral particles and dust are produced, lost or being transported through the system. These magnetic environments of the gas giants can be envisaged as huge plasma laboratories in space in which electromagnetic waves, current systems, particle transport mechanisms, acceleration processes and other phenomena act and interact with the large number of moons in orbit around those massive planets. In general it is necessary to describe and study the global environments (magnetospheres) of the gas giants, its global configuration with its large-scale transport processes; and, in combination, to study the local environments of the moons as well, e.g. the interaction processes between the magnetospheric plasma and the exosphere/atmosphere/magnetosphere of the moon acting on time scales of seconds to days. These local exchange processes include also the gravity, shape, rotation, astrometric observations and orbital parameters of the icy moons in those huge systems. It is the purpose of this chapter of the book to describe the variety of the magnetic environments of the outer planets in a broad overview, globally and locally, and to show that those exchange processes can dramatically influence the surfaces and exospheres/atmospheres of the moons and they can also be used as a tool to study the overall physics of systems as a whole.     

The Magnetic Field of the Milky Way from Faraday Rotation of Pulsars and Extragalactic Sources

Faraday rotation towards polarised pulsars and extragalactic sources is the best observable for determining the configuration of the magnetic field of the Galaxy in its plane and also at high latitudes. The Galactic magnetic field plays an important role in numerous astrophysical processes, including star formation and propagation of ultrahigh-energy cosmic rays; it is also an important component in measurements of the cosmological microwave background. This review article provides a brief overview of the latest advancements in the field, from an observer’s point of view. The most recent results based on pulsar rotation measures are discussed, which show that we have begun to confidently resolve the main features of the Galactic magnetic field on kiloparsec scales, both in the Solar neighbourhood and at larger distances. As we are currently in great anticipation of polarisation observations with new, state-of-the-art telescopes and hardware, a brief overview of how much this field of research will benefit from the upcoming pulsar surveys is also given.     

Radiation-driven diskons: An overview

The current status of the theory of a new astrophysical phenomenon, aradiation-driven diskon, is outlined.The cyclotron radiation pressure around sufficiently hot, strongly magnetized white dwarfs and neutron stars is shown to be able to drive a wind from the photosphere and support a plasma envelope in the closed part of the magnetosphere. The magnetohydrostatic configuration of an optically thin, radiatively supported plasma envelope is determined. It consists of an equatorial disk in the region where the cyclotron radiation force exceeds the local force of gravity and a closed shell near the equilibrium surface where the radiation pressure equals gravity. The effects of finite optical depth on the behaviour of the magnetospheric plasma and the influence of the envelope on the observed radiation are discussed.Classes of magnetic degenerate stars are pointed out in which radiation-driven diskons may be found. The best candidates are two individual stars, the strongly magnetized white dwarfs GD 229 and PG 1031+234. Both exhibit broad and deep depressions in the ultraviolet which are explained as a result of cyclotron scattering by an optically thick radiation-driven envelope in the inhomogeneous magnetic field of the star. We predict a temporal and spectral variability of these features due to non-stationary plasma motions in the envelope.