碳/碳复合材料导热性能的研究

对碳/碳复合材料在不同温度下的导热性能进行了研究。研究发现了碳/碳复合材料的导热机理介于金属材料和非金属材料之间,既有声子导热,又有电子导热。在实验温度范围内,导热系数随温度升高而增大。随碳/碳复合材料石墨化程度的增大,晶体微观结构渐趋完整,石墨片层的有序度增加,材料的导热性能增强。对于高密度的碳/碳复合材料,因为晶粒间联通状态良好,热传导载体运动的路径畅通,所以导热系数高。碳纤维及围绕纤维生长的热解碳是热传导的有效通道,所以沿纤维增强方向的导热系数高。     

同轴型微波等离子推力器磁场效应

在2.45 GHz同轴型微波等离子体推力器中加入磁场可以提高推力器的性能。这是由于磁场的存在,在推力器启动阶段会形成电子回旋共振区;稳定工作时,等离子体获得的焦尔热比没有磁场时高,这些都增加了等离子体吸收的微波能量。以氩气为工质,对外加磁场微波等离子推力器进行了实验研究,结果表明,推力器可以达到较高的耦合效率。对等离子体羽流的诊断则表明,外加磁场提高了推力器谐振腔内工质气体的电离度。     

超微粉（AlN＋Al）的添加对AIN的烧结和导热的影响

将混合超微粉（ＡｌＮ＋Ａｌ）添加到ＡｌＮ细粉中，在不同温度下进行了常压烧结试验。测定了烧结体的导热系数，进行了Ｘ射线衍射分析和电镜观察。结果表明：当烧结温度≤２０２３Ｋ时，超微粉的添加使ＡｌＮ的烧结密度和导热率提高；当烧结温度升至２１２３Ｋ时，超微粉的添加反而引起ＡｌＮ的烧结密度和导热率的下降。讨论了超微粉对ＡｌＮ的烧结和导热的作用条件和机理。     

射频离子推力器热特性仿真分析

为了分析射频离子推力器热特性，建立了射频离子推力器整体热模型，基于二维流体模型，对11cm射频离子推力器开展了放电室等离子体仿真，获得了电子温度、电势分布等关键参数；以等离子体仿真结果和实测束电流为输入，获得了各热源的热通量；通过有限元计算获得了关键部组件的温度分布，与实验结果进行了对比分析。研究结果显示：放电室内电子温度约为3.6eV~3.9eV，等离子体电势最高20V，发热损耗主要来自带电粒子轰击放电室壁面和栅极造成的能量沉积、激发原子的热辐射以及射频线圈自身的发热损耗，温度仿真与实测结果一致性良好，最大误差7%，仿真得到的温度分布可以作为输入参数进一步研究栅极受热形变及对束流的影响。     

Cosmological Shock Waves

Large-scale structure formation, accretion and merging processes, AGN activity produce cosmological gas shocks. The shocks convert a fraction of the energy of gravitationally accelerated flows to internal energy of the gas. Being the main gas-heating agent, cosmological shocks could amplify magnetic fields and accelerate energetic particles via the multi-fluid plasma relaxation processes. We first discuss the basic properties of standard single-fluid shocks. Cosmological plasma shocks are expected to be collisionless. We then review the plasma processes responsible for the microscopic structure of collisionless shocks. A tiny fraction of the particles crossing the shock is injected into the non-thermal energetic component that could get a substantial part of the ram pressure power dissipated at the shock. The energetic particles penetrate deep into the shock upstream producing an extended shock precursor. Scaling relations for postshock ion temperature and entropy as functions of shock velocity in strong collisionless multi-fluid shocks are discussed. We show that the multi-fluid nature of collisionless shocks results in excessive gas compression, energetic particle acceleration, precursor gas heating, magnetic field amplification and non-thermal emission. Multi-fluid shocks provide a reduced gas entropy production and could also modify the observable thermodynamic scaling relations for clusters of galaxies.     

SiC颗粒影响SiCp／Cu复合材料物理性能的研究

运用多元回归分析方法,研究了ＳｉＣ颗粒含量、粒度及纯度对ＳｉＣｐ／Ｃｕ复合材料热膨胀系数和导热率的影响规律。研究表明,影响材料热膨胀系数和导热率的主要因素为ＳｉＣ颗粒含量。随着ＳｉＣ颗粒含量的增加,复合材料的热膨胀系数和导热率降低;ＳｉＣ颗粒越小,热膨胀系数越低,而导热率越好;适当增加杂质含量有利于获得较高的导热率。     

Effects of Low Energetic Neutral Atoms on Martian and Venusian Dayside Exospheric Temperature Estimations

The heating of the upper atmospheres and the formation of the ionospheres on Venus and Mars are mainly controlled by the solar X-ray and extreme ultraviolet (EUV) radiation (λ = 0.1–102.7 nm and can be characterized by the 10.7 cm solar radio flux). Previous estimations of the average Martian dayside exospheric temperature inferred from topside plasma scale heights, UV airglow and Lyman-α dayglow observations of up to ∼500 K imply a stronger dependence on solar activity than that found on Venus by the Pioneer Venus Orbiter (PVO) and Magellan spacecraft. However, this dependence appears to be inconsistent with exospheric temperatures (<250 K) inferred from aerobraking maneuvers of recent spacecraft like Mars Pathfinder, Mars Global Surveyor and Mars Odyssey during different solar activity periods and at different orbital locations of the planet. In a similar way, early Lyman-α dayglow and UV airglow observations by Venera 4, Mariner 5 and 10, and Venera 9–12 at Venus also suggested much higher exospheric temperatures of up to 1000 K as compared with the average dayside exospheric temperature of about 270 K inferred from neutral gas mass spectrometry data obtained by PVO. In order to compare Venus and Mars, we estimated the dayside exobase temperature of Venus by using electron density profiles obtained from the PVO radio science experiment during the solar cycle and found the Venusian temperature to vary between 250–300 K, being in reasonable agreement with the exospheric temperatures inferred from Magellan aerobraking data and PVO mass spectrometer measurements. The same method has been applied to Mars by studying the solar cycle variation of the ionospheric peak plasma density observed by Mars Global Surveyor during both solar minimum and maximum conditions, yielding a temperature range between 190–220 K. This result clearly indicates that the average Martian dayside temperature at the exobase does not exceed a value of about 240 K during high solar activity conditions and that the response of the upper atmosphere temperature on Mars to solar activity near the ionization maximum is essentially the same as on Venus. The reason for this discrepancy between exospheric temperature determinations from topside plasma scale heights and electron distributions near the ionospheric maximum seems to lie in the fact that thermal and photochemical equilibrium applies only at altitudes below 170 km, whereas topside scale heights are derived for much higher altitudes where they are modified by transport processes and where local thermodynamic equilibrium (LTE) conditions are violated. Moreover, from simulating the energy density distribution of photochemically produced moderately energetic H, C and O atoms, as well as CO molecules, we argue that exospheric temperatures inferred from Lyman-α dayglow and UV airglow observations result in too high values, because these particles, as well as energetic neutral atoms, transformed from solar wind protons into hydrogen atoms via charge exchange, may contribute to the observed planetary hot neutral gas coronae. Because the low exospheric temperatures inferred from neutral gas mass spectrometer and aerobraking data, as well as from CO⁺ ₂ UV doublet emissions near 180–260 nm obtained from the Mars Express SPICAM UV spectrograph suggest rather low heating efficiencies, some hitherto unidentified additional IR-cooling mechanism in the thermospheres of both Venus and Mars is likely to exist. An erratum to this article can be found at     

Effect of Sintering on Thermal Conductivity and Thermal Barrier Effects of Thermal Barrier Coatings

Thermal barrier coatings (TBCs) are mostly applied to hot components of advanced turbine engines to insulate the components from hot gas. The effect of sintering on thermal conductivity and thermal barrier effects of conventional plasma sprayed and nanostructured yttria stabilized zirconia (YSZ) thermal barrier coatings (TBCs) are investigated. Remarkable increase in thermal conductivity occurs to both typical coatings after heat treatment. The change of porosity is just the opposite. The grain size of the nanostructured zirconia coating increases more drastically with annealing time compared to that of the conventional plasma sprayed coating, which indicates that coating sintering makes more contributions to the thermal conductivity of the nanostructured coating than that of the conventional coating. Thermal barrier effect tests using temperature difference technique are performed on both coatings. The thermal barrier effects decrease with the increase of thermal conductivity after heat treatment and the decline seems more drastic in low thermal conductivity range. The decline in thermal barrier effects is about 80 °C for nanostructured coating after 100 h heat treatment, while the conventional coating reduces by less than 60 °C compared to the as-sprayed coating.     

电磁波在等离子体高温气体中传输特性实验研究

针对高超声速飞行器头身部形成的等离子体鞘套对通信的影响,在中国空气动力研究与发展中心的粉末激波管上开展了电磁波在等离子体高温气体中传输特性的实验研究。实验中获得了等离子体气体中的电磁波透射率、电子密度和碰撞频率。实验结果表明：X波段和Ka波段电磁波在高激波马赫数Mas=16.1、1区气体压力P1=1200Pa的激波管实验状态下产生的厚度80mm等离子体高温气体中能量衰减大于30dB,难以传输;X和Ka波段电磁波在激波马赫数Mas=15.9、1区气体压力P1=80Pa的激波管实验状态下产生的厚度80mm等离子体高温气体中能量衰减大于30dB,难以传输;X波段和Ka波段电磁波在激波马赫数Mas=10.1、1区气体压力P1=80Pa的激波管实验状态下产生的高温等离子气体中平均传输损耗较小,可以进行有效传输;Ka波段电磁波在激波马赫数Mas=8.9、1区气体压力P1=1200Pa的激波管实验状态下产生的厚度80mm等离子体气体中平均传输损耗小于1dB,可以进行有效传输。实验得到的等离子体高温气体中的电磁波透射率、电子密度和碰撞频率与理论计算值基本一致。     

嵌金属丝端燃药柱燃烧过程的数值研究

通过对金属丝采用一维传热方程,对端燃药柱采用二维轴对称传热方程,对燃气采用常微分控制方程,数值研究了嵌金属丝端燃药柱发动机的工作过程和金属丝热物性及其直径对沿金属丝燃速的影响。计算结果表明,沿金属丝燃速随金属丝导热系数、金属丝熔点的增大而增大,随金属丝比热的减小而增大;对同种金属丝存在一个最佳金属丝直径,使沿金属丝燃速达到最大值。该模型计算结果与试验结果相符较好,且能够得到沿金属丝燃速、药柱燃面变化及燃气压力等随时间的变化;模型简单、所需计算资源较少,适用于工程设计应用。     

陶瓷热障涂层的隔热效果研究

通过理论公式推导和试验测量,得出 :热障涂层的隔热效果与环境温差成正比,但同等环境温差下涂层在更高的温度工作时,由于涂层材料导热系数的增大,其隔热效果减小。涂层厚度与隔热效果在实际涂层应用的厚度范围内也接近线性关系。随着发动机叶片冷却气流换热系数增大,热障涂层的隔热效果也越大,但两者并不是线性关系。涂层隔热效果随导热系数的减小而增大,并且在低导热系数区,热障涂层隔热效果对导热系数的变化更敏感。随着涂层的厚度增大,导热系数的改变所具有的增加涂层隔热效果的作用越大;但涂层越厚,单位厚度涂层导热系数改变所取得的隔热效果越低     

航空煤油RP-3结焦产物的物性

在环境温度为800K和900K条件下,获取RP-3航空煤油结焦产物,通过试验获得表观形貌及物性,拟合了结焦产物的比热容和导热系数随温度变化的经验关系式。结果表明:航空煤油结焦产物的微观结构为球状颗粒堆积且表面存在可见孔隙,表观密度约为1 049kg/m~3,真密度约为1 498kg/m~3,孔隙率约为29.9%,环境温度为800K下生成的油焦真密度较900K下生成的小;通过闪光法测得油焦比热容约为1.1~2.2J/(g·K),导热系数约为0.19~0.28W/(m·K),比热容和导热系数均随着温度的升高而增加,环境温度为800K下生成的油焦比热容和导热系数较在900K条件下生成的略大。     

磁控等离子体对尾喷管壁传热特性的影响

根据磁场作用下等离子体的湍流和传热能力将受到抑制的现象, 提出利用磁场控制低温等离子体隔离高温燃气与喷管壁的方法, 以减少高温燃气对壁面的传热, 从而达到降低壁面温度的目的.分别建立诱导磁场方程求解洛伦兹力和磁场作用下的k-ε湍流模型求解湍流粘度, 数值模拟了不同强度磁场作用下的磁控等离子体流动和传热特性.结果表明, 磁场能够有效地抑制湍流强度, 降低传热能力, 从而有效地降低壁面温度;并且磁场越强, 效果越明显.      

各向异性陶瓷基复合材料涡轮叶片概率性热分析方法

考虑陶瓷基复合材料等纤维增韧复合材料导热系数的各向异性及分散性,建立了基于概率统计的陶瓷基复合材料涡轮叶片热分析方法。研究中以Mark Ⅱ涡轮叶片冷却结构为例,综合利用有限元方法和蒙特卡洛方法,分析了应用陶瓷基复合材料后的温度场均值和波动特性。计算中将导热系数作为随机输入参数,分析了导热系数各向异性及其分散度对叶片前缘滞止点温度、尾缘温度以及高温区域（T>900K）面积的影响。计算中发现在本文的计算工况下,考虑导热系数存在正态波动情况时,叶片前缘滞止点、尾缘温度波动也满足正态分布。前缘滞止点温度在导热系数变异系数为01,导热系数比为2时其温度波动最大,相比12731K的均温,有16%的概率超温913K。尾缘温度在导热系数变异系数为01,导热系数比为10时波动最大,有16%的概率超过均值11529K达527K。计算结果表明:导热系数分散度所带来的波动,会导致叶片内部高温关注区域（T>900K）的面积增大,并且高温关注区域相对增加量ΔShot随导热系数变异系数α的增加而增加。计算结果表明,高温关注区域相对增加量最大发生在导热系数比为2,变异系数为0.1时,此时ΔShot=4.8%。      

微波与等离子体之间的相互作用

根据微波和等离子的基本理论以及它们之间相互作用的原理,建立了由微波能、谐振腔内电场、工质流场、等离子体平衡场等组成的轴对称偏微分方程组。通过对模型的计算,获得了放电管内等离子体区的形状、电场、电子浓度和温度场,以及气体温度场。     

基于电子束电离的磁流体力学进气道流动控制数值模拟

采用基于电子束电离的磁流体力学(MHD)控制系统,对高超声速流场附面层,以及非设计状态下的高超声速进气道流场的磁流体控制进行了深入研究.控制方程为低磁雷诺数Navier-Stokes方程,采用等离子体动力学模型与电子束模型模拟空气电离过程.研究结果表明:①电子束电离能有效提高流场的电导率,增强磁场对流场的控制效率;②基于电子束诱导电离的MHD控制系统能有效地控制高超声速流场的附面层,但其控制效率跟电子束能量大小相关;③基于电子束诱导电离的MHD控制系统能有效地改变非设计状态下高超声速飞行器的斜激波结构,使进气道重新满足Shock-on-lip(SOL)条件,但进气道的总压恢复系数以及流量将会降低.      

High-Energy Electron Beam Relaxation in a Stationary Plasma Thruster

In the paper, processes of high-energy electron beam interaction with plasma particles in a discharge channel of a stationary plasma thruster are analyzed and the results are presented.     

The Cassini Radio and Plasma Wave Investigation

The Cassini radio and plasma wave investigation is designed to study radio emissions, plasma waves, thermal plasma, and dust in the vicinity of Saturn. Three nearly orthogonal electric field antennas are used to detect electric fields over a frequency range from 1 Hz to 16 MHz, and three orthogonal search coil magnetic antennas are used to detect magnetic fields over a frequency range from 1 Hz to 12 kHz. A Langmuir probe is used to measure the electron density and temperature. Signals from the electric and magnetic antennas are processed by five receiver systems: a high frequency receiver that covers the frequency range from 3.5 kHz to 16 MHz, a medium frequency receiver that covers the frequency range from 24 Hz to 12 kHz, a low frequency receiver that covers the frequency range from 1 Hz to 26 Hz, a five-channel waveform receiver that covers the frequency range from 1 Hz to 2.5 kHz in two bands, 1 Hz to 26 Hz and 3 Hz to 2.5 kHz, and a wideband receiver that has two frequency bands, 60 Hz to 10.5 kHz and 800 Hz to 75 kHz. In addition, a sounder transmitter can be used to stimulate plasma resonances over a frequency range from 3.6 kHz to 115.2 kHz. Fluxes of micron-sized dust particles can be counted and approximate masses of the dust particles can be determined using the same techniques as Voyager. Compared to Voyagers 1 and 2, which are the only spacecraft that have made radio and plasma wave measurements in the vicinity of Saturn, the Cassini radio and plasma wave instrument has several new capabilities. These include (1) greatly improved sensitivity and dynamic range, (2) the ability to perform direction-finding measurements of remotely generated radio emissions and wave normal measurements of plasma waves, (3) both active and passive measurements of plasma resonances in order to give precise measurements of the local electron density, and (4) Langmuir probe measurements of the local electron density and temperature. With these new capabilities, it will be possible to perform a broad range of studies of radio emissions, wave-particle interactions, thermal plasmas and dust in the vicinity of Saturn.DeceasedThis revised version was published online in July 2005 with a corrected cover date.