无中和器射频离子推力器原理研究

在电推力器的广泛应用中,大部分都采用加速正离子的方式产生推力,且需要安装中和器发射电子对喷射出的正离子进行中和,否则会导致航天器自充电,对其通信及电子器件造成损害。因此,中和器的性能成为制约电推力器工作状态和寿命的重要因素。为了克服该缺点,介绍了一种基于同时加速正、负离子的无中和器射频离子推力器,阐述了其结构组成及推进原理,分析了离子-离子的产生、正负离子的加速过程,指出了关键技术包括电负性工质气体放电特性、磁场过滤电子束缚效能,以及可周期性交替加速正、负离子的栅极偏置电压加载方式。分析表明,该推力器在低轨航天器及深空探测器中具有潜在的应用前景。     

系缆气球的气动力估算和配平计算

从飞行力学分析的角度,用传统的气动力估算方式对具有倒"Y"型尾翼的系缆气球的气动力特性进行估算.考虑气球与系缆的综合系统,建立系缆气球平衡方程并进行配平计算.在不同的风速条件下,采用牛顿下降梯度法迭代求解非线性代数方程组形式的系缆气球平衡方程.通过不同风速及不同系缆位置的平衡状态的对比分析,确认系缆的最佳悬挂位置.      

银河宇宙线近地电荷成分

在1982年的气球飞行中, 球载塑料核径迹探测器CR-39在气球高度飞行了10小时.测得E>3.6GeV/n的银河宇宙线相对丰度, 结果与卫星探测数据基本一致.      

双系缆气球绳网系统的建模、配平及稳定性

为研究一种双系缆气球绳网系统的气球、绳网的设计问题和系统抗风能力的评估问题,建立了考虑风影响的双系缆气球绳网系统的数学模型,其中包括在体轴系下建立的气球的数学模型、根据无限细化理论建立的系缆的数学模型和按照一定的简化假设建立的绳网的数学模型;在配平状态下引入小扰动假设,使非线性方程组线化,并分析了该系统对阶跃风扰动的响应和稳定性.仿真计算结果表明该系统的设计合理并具有一定的抗风能力.      

磁层亚暴膨胀相的近地触发模型

本文指出现有亚暴的中性线模型其源区在赤疲乏面上离地球太远；以ＧＥＯＳ－２的观测资料为依据，提出了亚暴膨胀相的一个近地触发模型－气球模不稳定性模型，该模型认为，在增长相期间到达Ｒ≈（６－１０）ＲＥ的近地等离子体片内边缘区，出现指向地球方向的离子压强梯度，越尾电流强度增大，磁力线向磁尾拉伸。当等离子体片变薄，电子沉降增强，极光带电离层电导率骤增时，气球模不稳定性在近地等离子体片内边缘区被激发，场向电流     

高空科学气球的应力分析与球形设计

本文分析了迴转对称高空科学气球球膜的应力状态,指出按实际情况给定有关纬向应力σ_t的约束条件后就可解得正确的球形.σ_t的选择原则有三:下半球σ_t尽可能为零;上半球的σ_t自腰至顶逐渐增加;在球顶处则维持经向应力σ≈σ_t.按此原则设计的附加强带或不附加强带的气球,其最大应力和应力总潜能均较纬向应力恒为零的自然型气球有明显的改善,将用于大型气球的设计中.      

高空气球工作和学术会议

高空气球工作和学术会议由中国空间科学学会空间探测专业委员会和中国科学院有关单位联合召开的高空气球工作和学术会议于１９９４年４月１２日至１４月在北京举行．会议就高空气球科学探测和实验及高空气球技术进行了广泛的研讨，并对维持、发展我国高空科学气球事业的有...     

镜模波识别方法研究及其在火星磁鞘中的应用

镜模波是温度各向异性等离子体中的一种波动结构,根据磁场和离子分布及波动特性可以进行识别.本文对比了只使用磁场数据与同时使用磁场及离子数据两种识别方法,分析了两类方法的特点.只使用磁场数据的方法基于磁场强度变化大、方向沿背景磁场的特征,通常使用磁场强度的波动幅度ΔB/|B|以及磁场变化方向与背景磁场的夹角θ_min,θ_max作为参数;同时使用磁场及粒子数据的方法利用的是磁场纵波特性、总压平衡和波动在等离子体坐标系下静止的特征.使用两种方法对MAVEN卫星在火星磁鞘内的数据进行识别,结果表明在某些情况下,只使用磁场数据会导致对镜模波的误判.通过研究改变上述参数阈值时识别结果的变化,发现当θ_min> 40°,θ_max < 40°,ΔB/|B|> 80%时,只用磁场数据可取得较好的识别效果.      

高空气球热力学模型与上升过程仿真分析

基于对高空气球热力学环境的分析,建立了热力学与动力学耦合的高空气球动力学模型;并采用该模型对某高空气球的上升与驻留过程进行仿真分析.结果表明:高空气球上升过程中内部氦气存在"超冷"现象,其中平流层区域"超冷"明显,氦气平均温差为-19 K;由于"超冷",其上升速度曲线呈双"V"形变化;强太阳辐射与弱对流环境使驻留过程中氦气呈现"超热"现象,平衡时氦气平均温度比环境温度高39 K,球内氦气超压648.8 Pa.数值仿真的速度、平均温度变化规律与相关飞行试验数据相吻合,说明该仿真模型是有效的.      

Ion formation by high- and medium-velocities dust impacts from laboratory measurements and Halley results

The ion formation processes by dust impacts have been studied qualitatively as well as quantitatively by dust accelerator laboratory measurements. Iron, carbon and metallized glass particles in the femto- to nano-gram mass range had been impacted on various metal targets in a velocity regime of v = 2 - 64 km/s. In the high velocity regime as relevant for the (retrograde) Halley encounter more than 99% of the ions produced are singly charged atomic, the rest molecular ones. The ion/atom ratios are apparently modified SIMS yields, the modification parameter being impact velocity dependent. A semiempirical formula was deduced for the determination of mass and density of the impacting particle from target and projectile ion yields. When evaluating the Halley encounter results, the elemental distribution of p/Halley dust appeared nearly to be solar; the organic fraction (CHON) could be characterized in a rough manner as fairly unsaturated. Oligomers of the monomers C₂H₂ (65%), CH₂O (25%), and HCN (10%) are probable.

With medium velocities (for prograde comet encounter), i.e. v = 15-30 km/s molecular ion types govern the mass spectra. Consequently, more chemical information of the projectile can be expected in this case, additional to the elemental distribution. Mass and density of the impinging dust particles can be determined as well.     

Ion-conductivity measurements by a balloon-borne probe in the low latitude stratosphere

Three balloons were launched from Hyderabad, India in order to measure the electrical conductivity in the stratosphere. The measurements show that at the float altitude of around 34 km the positive ion conductivity is higher than the negative ion conductivity by a factor of 3 to 5 during daytime. In nighttime they differ by a factor of around 1.3. The conductivity values measured during one of the balloon flights (Apr. 1984) showed marked variations with time. It is suggested that these variations might have a weather related origin.     

Balloon-borne,high-altitude gravimetry

Gravity measurements from a high-altitude balloon can verify global and upward-continued gravity models. A gravimeter suspended beneath a balloon is in a dynamic, and largely unpredictable, environment sensing accelerations due to gravity and balloon motions. Independent measurements of balloon motions using inertial navigation data combined with ground tracking data will allow for separation of balloon-induced accelerations from gravitational accelerations. Analysis of these data must estimate: 1) vertical gravimeter accelerations due to motion and gravity, 2) horizontal velocity to estimate the Eötvös effect, and 3) gravimeter position for comparison with gravity models. The first engineering test flight occurred on 11 October 1983, during the seasonal wind reversal and was very successful. Flight duration was approximately seven hours, with two hours of data collected at each of 30 km and 26 km altitudes. The results include gravity estimates, design criteria for future flights and feasibility analysis for vertical gravity profiles during ascent and descent.     

Empirical model of the composition of the Venus ionosphere: Repeatable characteristics and key features not modeled

In-situ measurements of positive ion composition of the ionosphere of Venus are combined in an empirical model which is a key element for the Venus International Reference Atmosphere (VIRA) model. The ion data are obtained from the Pioneer Venus Orbiter Ion Mass Spectrometer (OIMS) which obtained daily measurements beginning in December 1978 and extending to July 1980 when the uncontrolled rise of satellite periapsis height precluded further measurements in the main body of the ionosphere. For this period, measurements of 12 ion species are sorted into altitude and local time bins with altitude extending from 150 to 1000 km. The model results exhibit the appreciable nightside ionosphere found at Venus, the dominance of atomic oxygen ions in the dayside upper ionosphere and the increase in prominence of atomic oxygen and deuterium ions on the nightside. Short term variations, such as the abrupt changes observed in the ionopause, cannot be represented in the model.     

中纬度冬季低热层潮汐水平风分量相位关系的MF雷达观测

采用武汉(30°N,114°E)MF雷达在2001年冬季的风场观测数据研究中纬度低热层大气潮汐水平风分量之间的相位关系.统一用弧度定义的各潮汐经纬向分量的拟合初相位在三个连续的高度上分别显示出相同的时间变化倾向和相近的相位差,但是在绝大多数观测时间△ψ24和△ψ12准正交,而△ψ8出乎意料地准同相.周日、半日和8 h潮汐经纬向分量的二次相位耦合(QPC)方程被分别估计出来,利用它们相减还得到一个潮汐相位差相关方程.推测的8 h潮汐相位和相位差与相应的观测值很好地符合.在第14个时间窗内,三个潮汐一般表现为椭圆偏振而不是圆偏振或线偏振,但是△ψ24和△ψ12在三个连续的高度上准正交,而△ψ8在92.0和94.0 km上准同相.因此估计的潮汐QPC方程、推导的潮汐相位差相关方程、观测的8 h潮汐准同相相位差以及典型的潮汐偏振图都是观测的周日、半日和8 h潮汐之间真实QPC的反映.      

自主火星探测高集成离子与中性粒子分析仪

小型化、高集成化是深空探测载荷发展的主要趋势。在我国自主火星探测计划中,设计了一种高集成化的火星离子与中性粒子分析仪。采用从传感器到电子学进行最大限度共用的设计思路,在一台仪器中实现对离子和能量中性原子进行能量、方向和成分的探测,大大降低了仪器对卫星平台的资源需求。仪器采取静电分析进行离子的方向和能量测量、采取飞行时间方法进行离子成分的测量。中性原子采用电离板电离成带电离子,后端的能量测量和成分测量与离子相同。鉴定件样机已经完成了初步的测试定标,结果表明其满足设计要求。     

Mass spectrometric measurements of stratospheric ions

Recent in situ measurements with balloon borne quadrupole mass spectrometers, between 20 and 45 km altitude, are reviewed and discussed.The major stratospheric positive ions observed are proton hydrates [H⁺(H₂O)_n] and non proton hydrates of the form H⁺X_m(H₂O)₂. The data analysis allows a derivation of the vertical mixing ratio profile of X (most probably CH₃CN), which is compared with recent model calculations. From negative ion composition data, showing the presence of NO₃^? and HSO₄^? cluster ions, the density of sulfuric acid in the stratosphere is deduced. The implications of these findings on our understanding of the sulfur chemistry is briefly treated.Finally some other aspects such as contamination, cluster break up and the use of stratospheric ion mass spectra for determination of thermochemical data and other minor constituents are discussed.     

Ion composition behaviour in low and mid-latitudes during high solar activity

In the present analysis, the mass spectrometer data from the ISS-b satellite, available in the form of contour plots at an average height of 1100 km for every alternate hour, is used. This analysis showed some interesting results in terms of the diurnal variation of the transition heights; at times dominance of He⁺ over the other ions, and the seasonal variations of different constituents. In the development of ion composition models, it is suggested that this type of result should be taken into consideration.     

Scientific ballooning in Japan – An over view of recent activities

Current status of scientific ballooning in Japan is reviewed. First, I describe successful application of balloon technologies to construct a vessel of transparent plastic film, to contain about 1000 tons of liquid scintillator in Kamioka Liquid Scintillator Anti-Neutrino Detector (KamLAND). KamLAND is a project to study neutrino oscillation phenomena, by detecting anti-neutrinos produced in distant nuclear reactors. Next, I describe high altitude balloons developed by the ISAS balloon group. They developed balloons made from ultra-thin polyethylene film, producing a balloon of volume 60,000 m³ which successfully reached an altitude of 53 km in 2002. This is a world record, the greatest altitude that a balloon has ever achieved. ISAS is applying further effort to develop balloons with even thinner films, to achieve a higher altitude than 53 km. Other recent activities by the ISAS balloon group are briefly described.I also review scientific ballooning projects now operating in Japan, particularly focusing on the Balloon-Borne Experiment with a Superconducting Spectrometer (BESS) program. This is a US–Japan collaborative program that has carried out very precise measurements of antiprotons, protons and other components in primary cosmic rays, as well as measuring the fluxes of atmospheric muons and other components. The results of these observations give us important information to improve our understanding of the production mechanism of antiprotons observed in the primary cosmic rays. The data are also important for analysis of atmospheric neutrino events observed by Super-Kamiokande and other ground-based neutrino detectors. Future prospects of BESS and other balloon-borne cosmic-ray research programs are also presented.     

Ionic mobility of the middle atmosphere

Positive ion mobilities are calculated for 40–75 km by computing the theoretical positive ion composition and combining it with laboratory-determined mobilities. Theoretical determinations for mobility appear to be especially apt for the 40–65 km region since oxonium ions are observed to be the principal positive ions and they should be subject to thermodynamic equilibrium. We compute a mean reduced mobility of 2.1 ± 0.1 cm²/V-s for 40–65 km using the 1976 U.S. Standard Atmosphere and a water vapor mixing ratio of 5 ppmv. The results are compared with atmospheric data for mobility. Observations of a lower mobility from about 35 km down to ground level are qualitatively compatible with the onset of the so-called non-proton hydrate ions at about this altitude and extending to lower heights. We note that the laboratory determined mobilities for oxonium ions average about 12 % less than the theoretical Langevin values. The total positive ion conductivity is determined also and compared with in-situ results.