一种增强数字万用表功能的高频电压测量电路

为了增强数字万用表对频率较高的电压信号的测量能力,加入一级自动采集、比较电路,从而实现对高频电压信号的峰值测量。     

涡喷式发动机尾焰红外辐射计算模型研究

根据射流场红外辐射理论,分别建立了轴对称和二元矩形喷管涡喷航空发动机尾焰在任一视线的辐亮度计算模型,利用该模型可对军用喷气式发动机尾焰外辐射进行计算评估,经测量验证,本模型计算结果与测量结果具有较好的一致性。     

多喷管液体火箭动力系统尾焰流场特性研究

为深入研究多喷管液体火箭动力系统尾焰流场特性,以由10台液体火箭发动机组成的多喷管动力系统为模型,采用耦合了Realizable k-ε湍流模型的N-S方程描述尾焰流动过程,考虑复燃反应的影响,并运用压力的隐式算子分割(PISO)算法进行求解,实现了以液氢液氧和液氧煤油为推进剂的两种不同发动机尾焰的混合计算,得到了不同飞行高度下火箭动力系统的尾焰流场结构及其参数分布情况。结果表明:随着飞行高度的升高,尾焰的膨胀角度越来越大,尾焰间的相互作用加强。由于复燃反应及尾焰间相互作用影响,尾焰流场会出现局部高温区域,同时火箭底部及喷管周围会出现旋流,旋流会卷吸尾焰高温燃气,从而会对火箭底部进行烧蚀,需要对其采取相应的热防护措施。     

火箭发动机喷焰对无线电信号传播的影响

一、前言火箭发动机喷焰是一种电子浓度和碰撞频率远比电离层高、湍动起伏异常剧烈的不均匀等离子体。火箭在高空飞行时,喷焰将形成比弹体大几倍、甚至几十倍的等离子体区域。当各种无线电信号穿过它时,均要受到移相和衰减,等离子体湍动又使信号的幅度和相位产生寄生调制。箭载天线受到喷焰影响时,性能要严重下降,甚至产生击穿现象。受火箭发动机喷焰影响的线路,轻则信号质量下降,给测量带来误差;重则信号完全中断,系统失效,测量不到数据。喷焰对信号的衰减,在几百兆赫遥测频段,最大可达30—40dB;在微波波段,     

液体火箭发动机尾焰复燃对红外辐射特性的影响

为深入研究液体火箭发动机尾焰复燃对红外辐射特性的影响,建立了一个适用于液体火箭尾焰复燃流场和红外辐射特性的计算模型。利用FLUENT软件计算液体火箭尾焰复燃流场,其中复燃反应采用有限速率化学反应模型;采用HITEMP数据库利用逐线积分法(LBL)计算尾焰气体的辐射气体参量;采用反向蒙特卡洛法(BMC)求解辐射传输方程,得到尾焰复燃流场的红外辐射特性。结果表明,复燃反应可大幅度改变尾焰流场特性,进而改变尾焰红外辐射特性。相比于冻结流,反应流流场温度和主要辐射气体含量最大增幅分别可达15.4%及47.5%,主要辐射波段内辐射强度最大增幅可达31.5%。随发动机飞行高度增加,复燃反应所引起的红外辐射强度增量随之降低。     

尖峰电压信号发生器的研制

尖峰电压信号发生器的核心是产生尖峰电压信号,通过CPU控制串联接入被试设备的供电电源的回路中,能够输出尖峰电压信号、电压浪涌信号的试验设备。本文将项目的阶段管理应用于尖峰电压信号发生器的研发中,以期更好的了解这些阶段,顺利实现既定目标。     

多喷管液体火箭动力系统尾焰冲击特性研究

为深入研究多喷管液体火箭动力系统尾焰冲击特性,以由多喷管液体火箭动力系统构成的发射平台为研究对象,采用三维N-S方程描述尾焰冲击流动过程,采用Realizable k-ε湍流模型封闭流动方程组,并运用压力的隐式算子分割(PISO)算法进行求解,得到了火箭动力系统尾焰对不同导流面导流槽的冲击流场参数。结果表明:导流面上受冲击影响最大的是沿喷管轴线方向的正冲击区域,且助推器尾焰对导流面的冲击效应相比于芯级更加强烈。锥形导流面对多喷管动力系统尾焰具有很好的引射和导流作用,相比于楔形导流面更能降低尾焰的冲击影响,但会在流场中形成漩涡并卷吸高温燃气,可能对发射系统造成破坏,需要增加相应的热防护措施。     

直流稳流电源输出纹波和噪声的测试方法

如何准确测量出直流稳流电源输出纹波和噪声是电源检定／校准工作中需要解决的问题。通过具体事例分析了用不同的测量设备测量同一台电源的纹波电压其结果不同的原因,提出了在测量稳流电源的纹波电压的过程中如何选择负载类型,为实际电源纹波测量工作提供了一些参考。     

固体燃料冲压发动机旋流燃烧特性试验

为研究固体燃料冲压发动机旋流燃烧特性,进行了直流与旋流对比直连式试验。固体装药内径40mm,长180 mm,成分为HTPB中加入65%的金属粉末。试验发动机采用火炬式点火器点火,空气由燃烧补氧式空气加热器加热至690 K,热空气流量300 g/s。试验测量了压力、推力等参数,使用监控录像对发动机尾焰进行拍摄,通过测量试验前后装药质量差获得固体燃料平均燃速。旋流试验未将旋流器伸入燃烧室即实现了火焰稳定,且旋流燃烧比直流燃烧表现出更好的稳定性,平均燃速较直流提高近50%。旋流燃烧尾焰存在明显的径向扩张,表明尾焰仍有切向动量,损失了部分推力。     

固体火箭喷焰对雷达测量信息的影响

从某系列四发固体火箭成功发射时的雷达跟踪测量数据发现：二级发动机关机前约３０秒存在测量数据随机误差由偏大、超差、直到严重超差的现象。本文给出了多种数据,并据此认为：其原因是各种射频信号通过具有高温弱等离子体的火箭喷焰区时,引起了衰减、相移和调幅调相噪声,给外弹道的无线电测量带来误差,且信号穿过喷焰区的路径越长,影响越大。     

内送粉超声速等离子喷涂流场特性分析

应用流体控制方程、传热传质方程、粒子输运方程、Maxwell电磁场方程建立多场耦合数学模型,通过数值计算方法研究超声速等离子喷枪内外等离子体流动特性。所采用的内送粉三维模型包含阴、阳电极固体以及阳极边界层区域,考虑了等离子气体的电离与复合反应,以及局域热平衡效应,得到了超声速等离子喷涂在纯氩和氩氢混合气氛中的气流温度场、速度场分布以及电弧电压分布。结果表明:在加入氢之后,喷枪内等离子体温度提高了30%,速度提高了67%;喷枪外气流速度和温度在距喷嘴出口0~50mm间梯度变化大于喷涂距离50~100mm,且径向速度和温度梯度变化随着喷涂距离增大越来越小。计算得到的电弧电压与测量值相差4.4%,说明了考虑阳极边界层后计算模型的合理性。     

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     

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。     

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。     

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.     

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.     

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。     

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     

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.