霍尔推进器磁屏蔽对磁场的优化效应研究

为研究磁屏蔽对霍尔推进器磁场位形分布的影响，以轴对称环形霍尔推进器为研究对象，采用FEMM软件对各种磁屏蔽情况下的磁场分布进行仿真；结合流体模型，利用四阶龙格库塔方法对放电通道内各粒子的输运性质进行研究。结果表明：内外磁屏蔽材料高度变化时磁场位形存在最优分布；电子温度在放电通道出口附近达到最大值，约64eV。离子化频率和电子轴向有效散射频率峰值也出现在通道出口附近。     

磁零点及通道宽度对霍尔推力器性能影响的数值研究

磁场位形和通道尺度会改变霍尔推力器等离子体放电过程,影响推力器的宏观放电特性。为分析磁场和通道宽度对推力器放电性能的影响规律,本文针对霍尔推力器轴对称通道结构和放电物理过程建立2D3V物理模型,采用粒子模拟方法研究了霍尔推力器磁零点磁场位形不同通道宽度的电势、粒子数密度、电子温度、电离速率、比冲及推功比的变化规律,结果表明：在具有磁零点磁场位形下,随着通道宽度增加,通道出口处电势降增加,加速区缩短,离子径向速度减少,壁面腐蚀降低;当磁零点位置在内壁面,推力器通道宽度由14 mm增加到16 mm时,推力器比冲和推功比增大,推力器放电效率提高;当磁零点位置在通道中轴线或外壁面,且通道宽度大于14 mm时,推力器比冲增大,推功比减小,推力器效率下降。     

霍尔推进器磁屏蔽对磁场的优化效应研究

为研究磁屏蔽对霍尔推进器磁场位形分布的影响,以轴对称环形霍尔推进器为研究对象,采用FEMM软件对各种磁屏蔽情况下的磁场分布进行仿真;结合流体模型,利用四阶龙格库塔方法对放电通道内各粒子的输运性质进行研究。结果表明:内外磁屏蔽材料高度变化时磁场位形存在最优分布;电子温度在放电通道出口附近达到最大值,约64eV。离子化频率和电子轴向有效散射频率峰值也出现在通道出口附近。     

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。     

LIPS-200环型会切磁场离子推力器热模型计算分析

为了建立国内自行研制的20cm口径LIPS-200环型会切磁场离子推力器放电室的热模型,研究了放电室内等离子体的产生过程,得到了二次电子的温度、离子密度以及电子密度分布规律,在此基础上得到放电室各个关键部件的电流沉积和能量沉积热模型。以热模型计算结果为依据,进行了推力器稳态工作下的有限元热分析以及热平衡验证试验。结果显示:推力器处于稳定放电时,放电室内电子温度分布范围为2~4e V;电离基本发生在放电室轴线附近,此处电离产生率和电子温度最高,并且整个放电室内离子密度约为1017/m3;放电室的内表面能量沉积主要来自二次电子及Xe离子。     

超大功率霍尔推力器放电参数影响仿真及试验

针对超大功率霍尔推力器放电参数特性评估,开展放电电压和流量等参数变化对性能影响的仿真及试验研究,以确定推力器设计最优匹配的放电电压及放电电流工况。建立了Particle-in-Cell(PIC)数值仿真模型,并搭建了HET-450大功率霍尔推力器试验平台;针对变放电电压、变流量下推力器放电特性,仿真计算给出了放电通道内原子密度、电势以及电子温度等分布,探究了推力器电离和加速运行机理,进一步,结合试验,开展了放电电流、推力等比对分析。结果表明：放电电压从300V增加至500V过程中,电离效率逐渐提升,因而放电电流、推力以及阳极效率均递增,而继续增加放电电压则会导致过热场的产生,离子与壁面作用增强导致电离出的离子再次复合,工质利用率下降的同时壁面损失增加,宏观表现为阳极效率的下降。此外,仿真与试验所获得放电电流、推力等结果符合良好,说明建模合适;在500V,80mg/s条件下,推力达2.1N、阳极效率60%,达到设计要求,表明设计合理有效。     

霍尔推力器通道宽度对电离特性的影响

为了研究霍尔推力器通道宽度对电离特性的影响,采用以数值模拟为主、实验验证为辅两种手段相结合的方式。所建立的数学模型是基于蒙特卡洛方法的二维完全动力学粒子模型,实验选择了与等离子体无接触的光谱诊断方法。计算和实验两方面的结果都发现随着宽度的增加,电子电离工质气体的速率增加,电离更加有效,而且电离区域变得集中的规律。通过进一步的计算发现,电离特性的明显差异和电子与壁面碰撞频率随宽度增加而减小,电子温度随之升高有着密切关系。电子温度升高一方面会对电离特性起到促进作用,另一方面也会使电离消耗的能量增加。由于稳态时的电子温度是由电子能量平衡机制决定的,因此对电子能量平衡方程进行深入分析之后发现,在研究通道宽度影响电离特性这一物理问题上,电子在壁面上的能量损失是决定电子温度的主导因素,而电离损失仅属于次要因素,宽度增加有利于改善推力器的电离特性。     

离子推力器放电室阳极壁面电流密度分布特性研究

为了准确掌握离子推力器放电室阳极壁面电流密度分布特性，并深入理解阳极壁面处等离子体运动特性，设计了近阳极壁面等离子体诊断的具体实施方案，并基于LIPS-200离子推力器开展了近阳极壁面处等离子体诊断试验研究，得到了主要磁极附近壁面等离子体参数，并得到阳极壁面吸收电流密度分布特性。试验结果表明：LIPS-200离子推力器阳极壁面处主要磁极附近的等离子体密度范围为，测试点的电子温度范围为，壁面电流密度范围为；柱段壁面电子温度相对锥段较低，但电流密度较大，尤其在中间极靴位置电流密度最大，约为阴极极靴处电流密度的3倍，约为屏栅极靴处电流密度的2倍，阳极电流主要在放电室中间极靴处发生损失。     

磁场对霍尔推力器放电特性及性能参数影响的粒子模拟研究

磁场强度及位形对霍尔推力器放电过程有显著影响。根据霍尔推力器通道尺寸和等离子体放电过程建立二维物理模型,采用粒子模拟方法,研究了不同磁场强度及位形等离子体放电特性,讨论了推力、推功比及放电电流的变化规律。模拟表明:当中轴线磁场强度峰值小于200G时,磁场对电子轴向传导约束减弱;当磁场强度峰值在200G～420G时,电子温度、电离率及电子与壁面碰撞频率降低,出口处离子径向速度增大,壁面腐蚀增加;当磁场强度峰值为280G时,加速区最短,放电电流最小。不同零磁点磁场位形会改变通道电离区和加速区位置,影响推力器放电性能。     

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。     

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.     

霍尔推力器能量损失系统性评价方法

霍尔推力器典型效率在50%左右,其余能量在电离、加速、耦合等过程中耗散掉,为了明确推力器优化设计的重点方向,需要定量地研究各个物理过程中损失的能量。因此,本文从能量损失分析的角度入手研究影响霍尔推力器效率的典型物理过程及机理,建立了针对霍尔推力器能量损失的系统性评价方法,为霍尔推力器设计及优化提供理论支撑。从霍尔推力器能量转化过程入手,并以能量的最终作用对象及性质作为分类的标准,建立了新的能量损失体系,认为霍尔推力器损失的能量主要有：径向羽流动能、阳极沉积热能、壁面沉积热能、电离能、阴极耦合损失。针对各项损失能量建立了实验评估方法,实验结果显示,阳极热沉积、壁面热沉积、羽流发散导致的能量损失是制约霍尔推力器效率的主导因素,其占比分别达到5.2%、24.7%、6.1%。实验测得所有输出功率占输入阳极放电功率比例达到102.1%,经不确定度分析,认为是阳极热沉积、电离能、阴极耦合损失的高估导致的,但该方法诊断得到的各项损失相对数量级关系是确定的,利用实验校核了方法的可行性,为霍尔推力器性能以及设计水平的评价提供了新的视角。     

微波在液体火箭发动机真空羽流中的衰减

为研究液体火箭发动机真空羽流对微波的衰减作用,以某双组元液体火箭发动机为对象,使用热力计算程序对燃烧室内的电子数密度进行了计算,使用冻 结假设和有限化学反应速率假设两种情况对喷管内带电粒子的电离和再结合过程进行了模拟,并对羽流中带电粒子数密度和5~30GHz微波穿过羽流的衰减量进行了估算.研究结果显示:该发动机燃烧室和喷管出口的电子数密度量级分别为 1013~1014cm-3和1010~1011cm-3,K,Na等碱金属为主要电子释放剂,Cl-,OH-等基团为主要电子吸收剂;低频微波在羽流中衰减更严重,5GHz微波的衰减可达4.5dB;微波斜穿羽流的衰减通常大于横穿情况.      

Energy Deposition in Planetary Atmospheres by Charged Particles and Solar Photons

We discuss here the energy deposition of solar FUV, EUV and X-ray photons, energetic auroral particles, and pickup ions. Photons and the photoelectrons that they produce may interact with thermospheric neutral species producing dissociation, ionization, excitation, and heating. The interaction of X-rays or keV electrons with atmospheric neutrals may produce core-ionized species, which may decay by the production of characteristic X-rays or Auger electrons. Energetic particles may precipitate into the atmosphere, and their collisions with atmospheric particles also produce ionization, excitation, and heating, and auroral emissions. Auroral energetic particles, like photoelectrons, interact with the atmospheric species through discrete collisions that produce ionization, excitation, and heating of the ambient electron population. Auroral particles are, however, not restricted to the sunlit regions. They originate outside the atmosphere and are more energetic than photoelectrons, especially at magnetized planets. The spectroscopic analysis of auroral emissions is discussed here, along with its relevance to precipitating particle diagnostics. Atmospheres can also be modified by the energy deposited by the incident pickup ions with energies of eV’s to MeV’s; these particles may be of solar wind origin, or from a magnetospheric plasma. When the modeling of the energy deposition of the plasma is calculated, the subsequent modeling of the atmospheric processes, such as chemistry, emission, and the fate of hot recoil particles produced is roughly independent of the exciting radiation. However, calculating the spatial distribution of the energy deposition versus depth into the atmosphere produced by an incident plasma is much more complex than is the calculation of the solar excitation profile. Here, the nature of the energy deposition processes by the incident plasma are described as is the fate of the hot recoil particles produced by exothermic chemistry and by knock-on collisions by the incident ions.     

Flow Field Investigation in a Trapezoidal Duct with Swirl Flow Induced by Impingement Jets

An enlarged model of trapezoidal duct near the leading-edge in the blade is built up. The effects of impingement jets, swirl flow, cross flow and effusion flow are considered. Experiments are performed to measure flow fields in this confined passage and exit holes on one of its side walls. Cross flow and effusion flow are induced in the channel by the outflow of side exit hole (SEH) and film cooling hole (FCH), which are oriented on one end wall and bottom wall of the passage. Detailed flow structures are measured for two impingement angles of 35° and 45° with 6 combinations of outflow ratios. Results show that the small jets impinge the target wall effectively while the large jets contribute to inducing and impelling a strong counter-clockwise vortex in the upper part of the passage. Cross flow plays a dominate role for the flow structures in the passage and exit holes. It deflects jets, enhances swirl and deteriorates side exit conditions. Impingement angle is another significant factor for the flow characteristics. Its effect reveals more evidently with cross flow. Within the present test conditions, the mass flow rates and outflow positions of FCHs have no distinct effect on the main flow structures.     

Langmuir双探针测量Hall推力器羽流特性

应用Langmu ir双探针测量了距离Hall推力器出口30~100 cm的羽流特性。实验中真空舱压力保持在5×10-4~2×10-3Pa之间。实验证明,电子温度和数密度随着角度和轴向距离的变化而变化,但羽流中远场的电子温度变化幅度很小,基本稳定在0.455 eV左右;电子数密度随着与轴向距离和中心轴夹角的增加而减小。实验结果可为高性能的Hall推力器设计提供参考依据,并为等离子体羽流的数值模拟提供输入条件和验证依据。     

电离层顶部电子含量对GNSS电离层层析的影响分析

卫星信号射线上的总电子含量(slant total electron content, STEC)是像素基全球卫星导航系统电离层层析(computerized ionospheric tomography, CIT)建模的必要数据来源，但电离层层析通常忽略1 000 km以上的顶部电子含量，为弄清这部分电子含量对层析结果的影响，利用NeQuick2模型计算站星视线上的STEC与其在电离层区域内的STEC比值来改正原始数据，并分别利用改正前后的STEC进行电离层层析。结果显示，电离层顶部电子含量占比约为10%，白天占比略大于黑夜，与测高仪站的数据相比，改正后的均方根值比改正前提高了20%以上；与Swarm卫星提供的电子剖面数据对比，改正后的层析结果精度较改正前提升了19.6%左右，且该方法受地磁扰动影响较为明显。总的来说，利用CIT进行小尺度电离层探测，可较直观地看出，顶部电子含量对层析结果的影响较大，需要采取相应手段予以剔除。     

New constitutive relation for eddy viscosity models

A new turbulent constitutive relation was directly derived from Boussinesq's hypothesis and mixing length theory, and then implemented in the standard k-ε model. The performance of this constitutive relation was validated in zero pressure gradient flat-plate boundary layer flow, fully-developed turbulent channel flow and separated flow in a plane asymmetric diffuser. The investigation demonstrated that, this new constitutive relation gave very accurate results in the former two basic cases and provided significant improvement in prediction of separated and reattachment points in the plane asymmetric diffuser. Separation and reattachment points at x/H=7.5 and 29 were calculated accurately in comparison to experimental results, and the static pressure coefficient of 0.82 was very close to large eddy simulation calculation. These results are very encouraging but further verification and extensive application of the new constitutive relation to other two-equation eddy viscosity model are needed.      

The Electron and ion Plasma Experiment for Fast

The ion and electron plasma experiment on the Fast Auroral Snapshot satellite (FAST) is designed to measure pitch-angle distributions of suprathermal auroral electrons and ions with high sensitivity, wide dynamic range, good energy and angular resolution, and exceptional time resolution. These measurements support the primary scientific goal of the FAST mission to understand the physical processes responsible for auroral particle acceleration and heating, and associated wave-particle interactions. The instrument includes a complement of 8 pairs of `Top Hat' electrostatic analyzer heads with microchannel plate (MCP) electron multipliers and discrete anodes to provide angle resolved measurements. The analyzers are packaged in four instrument stacks, each containing four analyzers. These four stacks are equally spaced around the spacecraft spin plane. Analyzers mounted on opposite sides of the spacecraft operate in pairs such that their individual 180° fields of view combine to give an unobstructed 360° field of view in the spin plane. The earth's magnetic field is within a few degrees of the spin plane during most auroral crossings, so the time resolution for pitch-angle distribution measurements is independent of the spacecraft spin period. Two analyzer pairs serve as electron and ion spectrometers that obtain distributions of 48 energies at 32 angles every 78 ms. Their standard energy ranges are 4 eV to 32 keV for electrons and 3 eV to 24 keV for ions. These sensors also have deflection plates that can track the magnetic field direction within 10° of the spin plane to resolve narrow, magnetic field-aligned beams of electrons and ions. The remaining six analyzer pairs collectively function as an electron spectrograph, resolving distributions with 16 contiguous pitch-angle bins and a selectable trade-off of energy and time resolution. Two examples of possible operating modes are a maximum time resolution mode with 16 angles and 6 energies every 1.63 ms, or a maximum energy resolution mode with 16 angles and 48 energies every 13 ms. The instrument electronics include mcp pulse amplifiers and counters, high voltage supplies, command/data interface circuits, and diagnostic test circuits. All data formatting, commanding, timing and operational control of the plasma analyzer instrument are managed by a central instrument data processing unit (IDPU), which controls all of the FAST science instruments. The IDPU creates slower data modes by averaging the high rate measurements collected on the spacecraft. A flexible combination of burst mode data and slower `survey' data are defined by IDPU software tables that can be revised by command uploads. Initial flight results demonstrate successful achievement of all measurement objectives.