湍流等离子体尾迹雷达散射截面的计算及其影响因素分析

针对一阶畸变波Born近似模型,深入分析了湍流内外尺度和电子数密度脉动值对雷达散射截面的影响,并且给出了关于湍流外尺度的一个经验的,能被工程上较好使用的公式.在以上分析的基础上,计算了几种高程条件下再入小钝头锥体等离子尾迹的雷达散射截面,与已有实验结果进行了对比分析.分析和计算结果表明,湍流的外尺度和局部电子数密度值对雷达散射截面值影响较大;湍流内尺度变化的影响不大.     

The consequences of micropulsations on geomagnetically trapped particles

Non-adiabatic radiation belt dynamics is largely controlled by interactions between geomagnetically trapped particles and various modes of plasma turbulence. Long period electric field fluctuations act as a major source mechanism for the inner zone through the process of inward radial diffusion of particles injected into the convection dominated outer zone. Higher frequency turbulence provides a major loss mechanism by pitch-angle scattering into the atmospheric loss cone. The wave particle interactions may take the form of self induced instabilities or parasitic scattering. Examples of each will be given in this review.     

MHD structures, waves and turbulence in the solar wind: Observations and theories

A comprehensive overview is presented of recent observational and theoretical results on solar wind structures and fluctuations and magnetohydrodynamic waves and turbulence, with preference given to phenomena in the inner heliosphere. Emphasis is placed on the progress made in the past decade in the understanding of the nature and origin of especially small-scale, compressible and incompressible fluctuations. Turbulence models to describe the spatial transport and spectral transfer of the fluctuations in the inner heliosphere are discussed, and results from direct numerical simulations are dealt with. Intermittency of solar wind fluctuations and their statistical distributions are briefly investigated. Studies of the heating and acceleration effects of the turbulence on the background wind are critically surveyed. Finally, open questions concerning the origin, nature and evolution of the fluctuations are listed, and possible avenues and perspectives for future research are outlined.     

Calculation of Wall Temperature for Aircraft Exhaust System with Considering Gas Radiation Heat Transfer

The coupled numerical simulation of flow field, solid temperature field, species concentration field and gas radiation transfer/ energy field based on statistical narrow-band correlated-k (SNBCK) model, is employed to accurately predict aerothermodynamic characteristic of aircraft exhaust system. A series of methods to increase computational efficiency and descend computational resources make it possible to finish the calculation in PC. The parameters of narrow-band model are evaluated by HITEMP line-by-line database. Three examples have proved the accuracy of using these methods to solve flow heat transfer coupled problem and radiation transfer/energy equation, which are the calculation of temperature distribution of water-cooling nozzle in rocket engine, the calculation of carbon dioxide absorptivity at 4.3 micron band, and the gas radiation heat transfer evaluation of the cylindrical furnace. Finally, the inner flaps temperature distribution of ejecting nozzle with floating outer flaps is computed, under high-altitude, high-speed and afterburning conditions. Two completely different air-inlet schemes of ejecting channel almost achieve the same effect in cooling inner flaps.     

Multi-Scale Plasma Turbulence in the Diffuse Interstellar Medium

I discuss how radioastronomical observations can provide information on the turbulence that governs the propagation of cosmic rays in the Galaxy. Interstellar radio wave propagation effects, collectively referred to as interstellar scintillations, yield information on the spatial power spectra of fluctuations in plasma density and magnetic field. Results of relevance to cosmic-ray physics are the existence of interstellar turbulence over a wide range of spatial scales (which can thus interact with a wide range of cosmic ray energies), the detection of magnetic field fluctuations in association with this turbulence, and a change in the nature of the turbulence on spatial scales of about 3.5 parsecs. A number of mysteries remain, such as the apparent suppression of Fast Magnetosonic wave generation by the interstellar turbulence.     

Microwave spectrum analysis as solar energy release diagnostics

The possibilities of using spectrographic observations of microwave radio emission as a solar flare plasma diagnostic are discussed. The spectral fine structure of the emission is interpreted in the context of plasma emission mechanisms. The balance equations for particles and plasma turbulence together with the transfer equations for electromagnetic waves in a plasma are solved for a model containing a diverging magnetic loop. As a result of the analysis of the blip-type spectral feature, the structure of energy release region and the unperturbed plasma concentration in the preflare loop are evaluated. The number of accelerated electrons and the intensity of the plasma turbulence in the source region are estimated using the properties of the weak continuum emission following the blip. Based on the degree of circular polarization of both the narrow band and the continuum emission, estimates for the external magnetic field strength and the angular width of the radiating plasma turbulence have been obtained.     

An Electrooptical Automatic Gain Control

The laser beam affords a valuable carrier medium for an optical calmunication system, but such a system for transmission through the atmosphere is subjected to wide fluctuations in received signal strength because of turbulence. An electrooptical automatic gain control system em has been studied and built which can substantially reduce the effect of these fluctuations. The effect of system parameters on the control characteristics are considered.     

Predicting near-wall turbulence with minimal flow units in compressible turbulent channel flows

Mach number effects on the near-wall turbulence in the absence of outer motions remain unclear so far. The present study extends the Minimal Flow Units (MFUs), a widely applied method to investigate near-wall turbulence free from the impact of large-scale motions in the outer region in incompressible channel flows, to compressible wall-bounded turbulence. The compressible near-wall turbulence in MFU proves accurate in replicating near-wall statistics, independent of Mach number and statistically equivalent to the universal signals extracted from the full-sized channel. It is further utilized as universal signals in the predictive models of compressible near-wall turbulence, which is capable of accurately predicting variances and joint probability density functions of velocity and temperature fluctuations.     

Plasma Diagnostics of the Interstellar Medium with Radio Astronomy

We discuss the degree to which radio propagation measurements diagnose conditions in the ionized gas of the interstellar medium (ISM). The “signal generators” of the radio waves of interest are extragalactic radio sources (quasars and radio galaxies), as well as Galactic sources, primarily pulsars. The polarized synchrotron radiation of the Galactic non-thermal radiation also serves to probe the ISM, including space between the emitting regions and the solar system. Radio propagation measurements provide unique information on turbulence in the ISM as well as the mean plasma properties such as density and magnetic field strength. Radio propagation observations can provide input to the major contemporary questions on the nature of ISM turbulence, such as its dissipation mechanisms and the processes responsible for generating the turbulence on large spatial scales. Measurements of the large scale Galactic magnetic field via Faraday rotation provide unique observational input to theories of the generation of the Galactic field.     

Plasmasphere Response: Tutorial and Review of Recent Imaging Results

The plasmasphere is the cold, dense innermost region of the magnetosphere that is populated by upflow of ionospheric plasma along geomagnetic field lines. Driven directly by dayside magnetopause reconnection, enhanced sunward convection erodes the outer layers of the plasmasphere. Erosion causes the plasmasphere outer boundary, the plasmapause, to move inward on the nightside and outward on the dayside to form plumes of dense plasma extending sunward into the outer magnetosphere. Coupling between the inner magnetosphere and ionosphere can significantly modify the convection field, either enhancing sunward flows near dusk or shielding them on the night side. The plasmaspheric configuration plays a crucial role in the inner magnetosphere; wave-particle interactions inside the plasmasphere can cause scattering and loss of warmer space plasmas such as the ring current and radiation belts.     

Type-III radio bursts and their interpretation

The observations of type-III solar radio bursts are briefly reviewed to set requirements on a model for their interpretation. The most important of these requirements is that the source must be an electron stream which is in a state of continuous quasilinear relaxation and which initially must have a nearly monotonically decreasing velocity distribution. The problem of constructing a model is broken into three parts: (1) The plasma wave source which depends on the interaction of the electron stream with electron plasma waves. (2) The radiation source which depends on the interaction of plasma waves and transverse electromagnetic waves or in a magnetized plasma the ordinary and extraordinary modes of magnetoionic theory. (3) The propagation of radiation between the source and the observer which depends on the transmission of radiation through a scattering refracting absorbing magnetized plasma.Progress on a model for the plasma wave source is reviewed and it is concluded that no existing models are adequate. The equations which would lead to an adequate model are written down, but not solved. These include, in addition to collisional damping, Landau damping both by the exciting stream and the background plasma, and spontaneous and induced processes for a three-dimensional distribution of plasma waves. Possible limitations to a quasilinear approach such as pile-up of plasma waves and nonlinear effects are considered. Processes which affect the gross structure of the source such as electron trajectories in coronal streamers and electron scattering by inhomogeneities are reviewed.Progress on the radiation source is considered both in the absence and presence of a magnetic field. At high frequencies (e.g., 80 MHz) observations of radiation near the fundamental and second harmonic of the plasma frequency allow a unique determination of source size and the energy density in plasma waves within the uncertainties of geometry by source ray tracing. This determination is extremely critical because the fundamental must be amplified and thus production of the fundamental is effectively a much more highly nonlinear process than production of the second harmonic. At low frequencies (e.g., 500 kHz) the second harmonic is shown to be dominant because amplification of the fundamental becomes an inefficient process.Calculations of scattering of radiation in a random medium are reviewed. It is concluded that these are adequate at high and low frequencies, but have not been carried out properly at intermediate frequencies where amplification of the fundamental may still be present. It is shown in particular that when scattering is taken into account at high frequencies all observations can be explained by isotropic emission near the second harmonic. At low frequencies the nature of the scatterers is determined by source occultations unlike the case at high frequencies where these are free parameters. This fact allows the possibility of determining true source sizes at low frequencies by subtracting out the contribution due to scattering. A mechanism for producing the possibly observed linear or highly elliptical polarization of type-III bursts, which must be imposed far from the source due to Faraday rotation, is reviewed.Finally, the questions of what remains to be done and what we can hope to obtain upon completion of this work are briefly considered.The National Center for Atmospheric Research is sponsored by the National Science Foundation.     

螺旋式发射管内火箭燃气冲击流场数值模拟

用改进的MUSCL格式解三维、可压缩平均雷诺纳维尔-斯托克斯方程组,湍流模型为Spalart-Allmaras代数模型,计算和分析了火箭发射管内燃气冲击流场.在建立差分算法时,将有限体积离散和黎曼解算器相结合,简化了计算工作.首先,以小喉截面超声速喷管流动问题开展数值实验,数值结果与实验数据吻合很好;其次,计算了火箭发射管内燃气流场,获得发射管内气流压强和温度等物理参数分布.     

SH波对结构表面上含有多个半圆形介质夹杂的散射

利用复变函数和多极坐标系的方法,研究了在结构表面上含有多个半圆形介质夹杂的散射问题,首先给出 SH波对多个半圆形介质夹杂的散射波函数,并利用多极坐标系的方法,来满足介质界面上的连续条件和表面上的边界条件,归结为对一组无穷代数方程组的求解,简化了问题的求解。作为算例,对结构水平面上含有 2个半圆形夹杂介质进行分析,并讨论了夹杂介质参数的变化及孔距对位移的影响。     

液体火箭发动机尾焰对发射平台冲击效应

为研究液体火箭发动机尾焰对发射平台的冲击效应特性,建立液体火箭发动机尾焰对发射平台冲击数值计算模型.针对液氧/煤油发动机尾焰对发射平台冲击特性,基于建立模型研究了喷管出口距离平台3,5m工况下推进剂流量和复燃对冲击特性的影响,并分析了影响差异及其产生差异的原因.结果表明:尾焰自由射流区的激波膨胀、压缩距离和壁射流区面积随推进剂流量的增大而增大;考虑复燃化学反应不仅改变了自由射流区和滞止区的形状结构,而且增大了壁射流区的面积和温度;复燃和推进剂流量均是通过影响尾焰结构对冲击特性产生影响,具体影响效果与喷管出口和发射平台间距离有关.      

基于旋翼下洗流场的直升机动力舱通风冷却系统仿真

本文对直升机悬停状态下下洗流场影响区域、动力舱以及发动机排气引射器进行了联合建模,采用结构化网格对计算域进行离散,采用有限体积法求解雷诺平均Navier-Stokes方程,通过数值仿真考察不同湍流模型、发动机散热、以及动力舱进口尺寸对排气引射器引射系数以及动力舱通风冷却系统内部流场的影响。结果表明,引射系数对湍流模型依赖性较小;发动机散热将导致引射气流量、引射系数减小,而且随着冷却气流进口面积的增大,这种影响将增大;增大冷却气流进口尺寸,冷却气流量增大,引射系数增大,但进口尺寸增大到一定值后,其效果已不明显。     

Langmuir Turbulence and Solar Radio Bursts

Langmuir waves and turbulence resulting from an electron beam-plasma instability play a fundamental role in the generation of solar radio bursts. We report recent theoretical advances in nonlinear dynamics of Langmuir waves. First, starting from the generalized Zakharov equations, we study the parametric excitation of solar radio bursts at the fundamental plasma frequency driven by a pair of oppositely propagating Langmuir waves with different wave amplitudes. Next, we briefly discuss the emergence of chaos in the Zakharov equations. We point out that chaos can lead to turbulence in the source regions of solar radio emissions. This revised version was published online in August 2006 with corrections to the Cover Date.     

火箭发动机燃气射流流场的光学显示方法研究

本文研究了两种用于真实固体火箭发动机燃气自由射流流场和射流冲击流场显示的光学方法。实验结果表明 ,等厚条纹型 F- P干涉法。能够用于燃气自由射流流场的显示 ,而莫尔偏折法除此之外还可用于大范围的燃气射流冲击流场的显示。由此解决了长期以来无法显示这种高温、高压、强冲击、强火焰光等恶劣环境条件下的流场问题     

非对称交叉激波和湍流边界层相互作用的数值研究

针对7°×11°双尖鳍外形的非对称交叉激波与湍流边界层相互作用,采用Navier-Stokes方程和5种湍流模型进行了计算.主要考察对壁面压强、热传导、绝热壁面温度和壁面摩擦力线分布的计算精度.计算结果表明:两道斜激波相交后的区域的壁面压强和热传导都比较高;计算的压强和壁面摩擦力线与试验吻合很好,绝热壁面温度次之,热传导最差,峰值高达试验的3倍左右.湍流模型对壁面压强和壁面摩擦力线影响很小,对绝热壁面温度和热传导影响很大.在5种湍流模型中,TNT(turbulent/non-turbulent)和SST(shear-stress transport)模型表现较好.      

聚心火焰与诱导激波相互作用及爆燃转爆轰过程

基于带化学反应的二维轴对称Eu ler方程,利用带限制函数的波传播算法,在两端均敞开和一端封闭一端敞开的两种边界情况下,对圆柱型燃烧室中的氢气-空气预混气的聚心燃烧进行了数值模拟,探讨了聚心火焰引发爆轰过程中的波系结构以及火焰的变形。数值结果表明,在两端均敞开的情况下,燃烧诱导的激波在轴心、火焰和壁面之间来回反射,使火焰失稳,加速了火焰的燃烧,但没有转变成爆轰。而在一端封闭的情况下,封闭端反射产生的激波,不断穿越火焰,使火焰严重失稳,加剧了燃烧速度,最终导致爆轰的形成。稳定爆轰阵面的参数与CJ理论计算的结果进行了对比,两者符合的较好。同时,火焰在与激波的作用过程中,形状扭曲变形,对于两端敞开的情况呈对称的扁平头部蘑菇云,而对于一端封闭的情况,则呈封闭端小敞口端大的扁平头部蘑菇云。