超声速等离子喷涂颗粒加热熔化与细化过程分析

针对超声速等离子喷涂过程中颗粒撞击基体前熔化状态未知的问题,利用数值计算方法分析了单个颗粒在超声速气流中的加热熔化过程,并对颗粒的破碎细化行为进行了探究。计算考虑颗粒内部相变后,得到不同时刻颗粒内部的温度分布更加合理,通过分析得到了颗粒熔化界面随加热时间的变化曲线,其在0.35ms时完全熔化,这与实验分析结果相符。熔融颗粒在进入到高温高速等离子体射流中粒径会迅速减小,统计得到100mm处小于5μm的颗粒所占比例最大,超过了50%,与实验收集粒子的粒度分布一致。     

等离子体气动激励控制超声速边界层分离的实验研究

等离子体气动激励与超声速气流相互作用已成为高速流动控制领域的研究热点。激波与边界层相互作用现象广泛存在于超声速飞行器之中。本文进行了等离子体气动激励控制压缩角区和激波诱导边界层分离的实验,通过流场纹影显示和壁面静压测量,研究等离子体气动激励如何影响激波、激波如何影响边界层特性的科学问题。实验结果表明:施加毫秒量级表面电弧放电能够前移压缩角区的诱导斜激波,使分离区后移,分离区域增加,但激波强度减弱,流场总压增加;施加微秒量级表面电弧放电能够抑制激波诱导边界层分离,使分离区减小,流场总压减小。基于实验结果,认为毫秒量级表面电弧放电激励控制超声速气流的主要机理为放电过程的焦耳热效应;微秒量级表面电弧放电激励控制超声速气流的主要机理为焦耳热效应和冲击波效应共同作用。     

新的航空发动机零部件维修方案——K3冷喷涂工艺

<正>K3冷喷涂工艺与其他喷涂工艺的最大区别在于,其喷涂温度低于喷涂材料的熔点,喷涂速度为超声速,因此其最大的应用前景是用于航空发动机零部件的维修与修理。常规的热喷涂工艺包括等离子喷涂、火焰喷涂、高速火焰喷涂和金属丝电弧喷涂等。K3冷喷涂工艺是一种正在研发的新的热喷涂工艺,其全称为K3气动冷气喷涂工艺(K3-kinetic cold gas spraying process)。与其他热喷涂工艺的最大区别在于,K3冷喷涂工艺的喷涂温度低于喷涂材料的熔点,喷涂速度为超声速。因此也为K3冷喷涂工艺带来了巨大的应用优势,尤其是在航空发动机零部件的维修与修理上有着广泛的应用前景。K3冷喷涂工艺的基本工作原理是,将气体(如氩气、氦气和氮气)压缩并加热到800℃,然后通过拉伐尔形喷嘴以超声速喷出,借助载气(工作气流)将     

自制等离子喷枪冷却系统的设计及测试

等离子喷枪是制备热障涂层中的研究重点。目前关于等离子喷枪的研究多集中于喷嘴(阳极)、阴极,鲜有关于喷枪冷却系统方面的研究;喷枪冷却系统的优劣直接影响喷枪的工作寿命和喷涂过程的稳定性,同时制备热障涂层的质量也与冷却效果紧密相关。本文利用三维模型,详细阐述了自制的喷枪冷却系统通道及工作原理,并对设计进行了理论计算,对自制的喷枪进行点火试验和喷涂测试,结果显示自制的喷枪冷却系统功能良好,喷枪工作稳定,涂层质量较好。     

K3冷喷涂与等离子喷涂和超声速火焰喷涂的区别

<正>等离子喷涂设备及工艺是采用等离子弧发生器(喷枪)将通入喷嘴内的气体(常用氩气、氮气和氢气等)加热和电离,形成高温高速等离子射流,熔化和雾化金属或非金属喷粉,并使其以高速喷射到经预处理的工件表面上形成涂层的方法。超声速火焰喷涂是应用火箭发动机的原理获得温度较低(3400K)、但速度却很高的喷涂燃流。其突出的贡献是大幅度提高了涂层的结合强度、密度、硬度,同时降低了涂层中的氧化物含量,使涂层较等离子喷涂更加纯净。此外,超声     

高密度烃燃料雾化特性试验

采用试验手段研究了高密度烃燃料在直射式喷嘴情况下的雾化规律,采用数字图像处理技术,使用粒子图像测速系统（PIV）对其在横向高温气流中形成的喷雾场进行图像测量和分析。初步研究了气流温度、油压、气压与气流速度对高密度烃燃料雾化特性的影响,以及射流与喷嘴距离对喷雾粒子索太尔平均直径（SMD）的影响。试验结果显示：气流温度和油压的增加有助于提高高密度烃的雾化效果。在研究气流速度对其影响时,要考虑加热气流蒸发产生的影响,在雾化初始阶段速度因素占主导地位,而在下游距离喷嘴50~75mm间的某一位置开始,蒸发因素将起到主要作用。通过数值计算与实验比较,进一步说明了高温气流蒸发作用在颗粒二次雾化中的重要性。研究结果为优化设计高密度烃燃料发动机燃烧室提供依据。     

阳极通道长度对等离子体射流点火器特性影响的实验研究

为进一步优化等离子体射流点火器的结构,提高点火器的工作性能,在自主设计的等离子体点火实验系统的基础上,开展了阳极通道长度对等离子体射流点火器特性影响的实验研究,选取的阳极通道长度为3mm,5mm和7mm。获得了等离子体射流点火器的放电特性、光谱特性、射流特性和点火特性。结果表明:增大阳极通道长度能够抑制电弧分流的幅度,减小电极的烧蚀面积,但提高了击穿电压,使引弧更加困难;随着阳极通道长度的增大,氮分子离子的转动温度和振动温度分别呈现出先升高后降低和先降低后升高的变化趋势;煤油/空气混合气的点火延迟时间随阳极通道长度的增加,呈现出先减小后增大的变化趋势,余气系数为1.43时,阳极通道长度5mm时的点火延迟时间为14.4ms,相对于阳极通道长度3mm,7mm下的点火延迟时间分别减小了21.1%,12.1%。     

电弧放电等离子体激励控制超声速压气机叶栅激波/边界层干扰仿真研究

为研究电弧放电等离子体激励对超声速压气机叶栅激波/边界层干扰的控制作用,建立了模拟等离子体激励作用效果的唯象学模型,进一步以ARL-SL19超声速叶栅为对象,通过数值仿真研究了电弧放电等离子体与叶栅通道内部流动的相互作用及其对叶栅流动损失的影响。结果表明:等离子体唯象学模型能够较好模拟电弧放电等离子体诱导产生冲击波的气动特性。电弧放电等离子体激励对叶栅通道内部流动主要具有三种作用效果:在放电区,注入的热量会产生阻塞效应,增加近壁面气流的流动损失;在激波/边界层相互作用区,能够改变激波系结构,减小激波损失;在尾迹区,冲击波会诱导产生脱落涡。     

电弧加热流场湍流度对尖锥边界层转捩影响的研究

电弧加热流场的热环境特性直接影响热防护系统的地面试验数据,由于电弧加热器高温气流和参数波动的原因,直接测量湍流度非常困难。为研究电弧加热流场湍流度对于边界层转捩的影响,采用红外热图热像仪,在电弧加热流场中进行了5°尖锥模型边界层转捩研究。结合数值计算,将试验结果与常规风洞的尖锥边界层转捩结果进行了比较。结果表明：马赫数影响的雷诺数转捩判别准则可以用于计算电弧加热流场的转捩雷诺数;电弧加热流场的尖锥边界层转捩雷诺数显著小于常规风洞的转捩雷诺数,表明在该试验条件下,电弧加热流场的湍流度显著大于常规风洞。     

复杂型面自动喷涂关键技术研究

针对航空零件复杂型面进行自动喷涂关键技术研究,在总结人工喷涂工艺的基础上,计算喷涂房风量、等离子喷枪喷涂距离和喷涂位姿对羟基磷灰石涂层的影响,设计开发航空零件复杂型面自动喷涂单元,实现航空复杂零件的自动化喷涂,提高产品质量和稳定性,减少环境污染。     

美国等离子隐身研究和等离子空气动力学的新进展

美国等离子技术的研究进一步证实,等离子流可以用于飞机的隐身和改进流场,关键是能够获得低功率的机载等离子发生器。这里介绍的是美国研究机构在研究低功率等离子发生器以及用等离子改进飞机空气动力流场方面取得的一些最新进展     

穿孔等离子弧焊尾焰电压的检测

提出了一种简便实用的尾焰电压检测方法,可直接测量建立于工件与测量板之间的尾焰电压信号。该信号能准确反映熔池小孔的状态。     

等离子体激励式压气机

受吴仲华先生"叶轮机械三元流动理论"的启发,在前期压气机等离子体流动控制研究的基础上,进一步提出等离子体激励式压气机的概念,即将等离子体激励融入到S1,S2流面压气机气动设计之中,以释放常规压气机设计中失速裕度、负荷极限等因素的约束。本文旨在探讨等离子体流动控制在新一代高负荷压气机中应用的前景和研究趋势,通过原理论证与实例分析,首先阐述了等离子体激励式压气机的概念,然后梳理了压气机等离子体流动控制研究的若干进展,以论述等离子体激励式压气机设计的研究基础,最后给出了等离子体激励式压气机的典型技术路径和理论基础。     

等离子体隐身技术浅议

当今,新型隐身兵器不断问世,新的隐身机理相继出现。本文主要论述等离子体隐身技术的基本概念及对雷达波的隐身机理。     

Cassini Plasma Spectrometer Investigation

The Cassini Plasma Spectrometer (CAPS) will make comprehensive three-dimensional mass-resolved measurements of the full variety of plasma phenomena found in Saturn’s magnetosphere. Our fundamental scientific goals are to understand the nature of saturnian plasmas primarily their sources of ionization, and the means by which they are accelerated, transported, and lost. In so doing the CAPS investigation will contribute to understanding Saturn’s magnetosphere and its complex interactions with Titan, the icy satellites and rings, Saturn’s ionosphere and aurora, and the solar wind. Our design approach meets these goals by emphasizing two complementary types of measurements: high-time resolution velocity distributions of electrons and all major ion species; and lower-time resolution, high-mass resolution spectra of all ion species. The CAPS instrument is made up of three sensors: the Electron Spectrometer (ELS), the Ion Beam Spectrometer (IBS), and the Ion Mass Spectrometer (IMS). The ELS measures the velocity distribution of electrons from 0.6 eV to 28,250 keV, a range that permits coverage of thermal electrons found at Titan and near the ring plane as well as more energetic trapped electrons and auroral particles. The IBS measures ion velocity distributions with very high angular and energy resolution from 1 eV to 49,800 keV. It is specially designed to measure sharply defined ion beams expected in the solar wind at 9.5 AU, highly directional rammed ion fluxes encountered in Titan’s ionosphere, and anticipated field-aligned auroral fluxes. The IMS is designed to measure the composition of hot, diffuse magnetospheric plasmas and low-concentration ion species 1 eV to 50,280 eV with an atomic resolution M/ΔM ∼70 and, for certain molecules, (such asN ₂ ⁺ and CO⁺), effective resolution as high as ∼2500. The three sensors are mounted on a motor-driven actuator that rotates the entire instrument over approximately one-half of the sky every 3 min.This revised version was published online in July 2005 with a corrected cover date.     

The Near-Earth Plasma Environment

An overview of the plasma environment near the earth is provided. We describe how the near-earth plasma is formed, including photo-ionization from solar photons and impact ionization at high latitudes from energetic particles. We review the fundamental characteristics of the earth’s plasma environment, with emphasis on the ionosphere and its interactions with the extended neutral atmosphere. Important processes that control ionospheric physics at low, middle, and high latitudes are discussed. The general dynamics and morphology of the ionized gas at mid- and low-latitudes are described including electrodynamic contributions from wind-driven dynamos, tides, and planetary-scale waves. The unique properties of the near-earth plasma and its associated currents at high latitudes are shown to depend on precipitating auroral charged particles and strong electric fields which map earthward from the magnetosphere. The upper atmosphere is shown to have profound effects on the transfer of energy and momentum between the high-latitude plasma and the neutral constituents. The article concludes with a discussion of how the near-earth plasma responds to magnetic storms associated with solar disturbances.     

Plasma waves at Venus

Many significant wave phenomena have been discovered at Venus with the plasma wave instrument flow on the Pioneer Venus Orbiter. It has been shown that whistler-mode waves in the magnetosheath of the planet may be an important source of energy for the topside ionosphere. Plasma waves are also associated with thickening of the ionopause current layer. Current-generated waves in plasma clouds may provide anomalous resistance resulting in electron acceleration, possibly producing aurora. Ion-acoustic waves are observed in the bow shock, and appear to be a feature of the magnetotail boundary. Lastly plasma waves have been cited as evidence for lightning on Venus.     

温度、密度对目标等离子体隐身效果影响的FDTD分析

采用等温近似,给出覆盖目标的不均匀的、各项同性的、热的、碰撞的、等离子体的电磁反射的三维FDTD算法的公式。在一维条件下,计算了不同密度分布、不同温度的等离子体对电磁波的反射系数。给出了温度、密度对电磁波在等离子体中的碰撞吸收的影响。结果显示,增大等离子体的温度和密度将有利于等离子体对电磁波的吸收,增大吸收的带宽,减小等离子体覆盖目标对电磁波的反射。     

Plasma Properties in Coronal Funnels

A two dimensional model of the transition region and the lower corona, based on the idea that the magnetic flux is strongly concentrated at the boundaries of the supergranular convection cells, has been proposed by Gabriel in 1976. The plasma moves along the open magnetic field lines, which define the the so-called "funnel," and eventually builds up the solar wind. Based on a two dimensional funnel model we investigate the stationary plasma flow at its central line, taking heat conduction, radiative losses, and a heating function into account. The derived height profiles of the plasma properties within the funnel are presented. This revised version was published online in June 2006 with corrections to the Cover Date.     

The Galileo Plasma wave investigation

The purpose of the Galileo plasma wave investigation is to study plasma waves and radio emissions in the magnetosphere of Jupiter. The plasma wave instrument uses an electric dipole antenna to detect electric fields, and two search coil magnetic antennas to detect magnetic fields. The frequency range covered is 5 Hz to 5.6 MHz for electric fields and 5 Hz to 160 kHz for magnetic fields. Low time-resolution survey spectrums are provided by three on-board spectrum analyzers. In the normal mode of operation the frequency resolution is about 10%, and the time resolution for a complete set of electric and magnetic field measurements is 37.33 s. High time-resolution spectrums are provided by a wideband receiver. The wideband receiver provides waveform measurements over bandwidths of 1, 10, and 80 kHz. These measurements can be either transmitted to the ground in real time, or stored on the spacecraft tape recorder. On the ground the waveforms are Fourier transformed and displayed as frequency-time spectrogams. Compared to previous measurements at Jupiter this instrument has several new capabilities. These new capabilities include (1) both electric and magnetic field measurements to distinguish electrostatic and electromagnetic waves, (2) direction finding measurements to determine source locations, and (3) increased bandwidth for the wideband measurements.Deceased